research annual report 2013 - cas · annual report’ î ì í3－content iii (50) constraints on...

Research Annual Report

科

研

工

作

年

度

报

告

2013

中国科学院紫金山天文台

2013 科研工作年度报告

中国科学院紫金山天文台科技处

2014 年 4 月

Cover: Local Arm probable major branch of Perseus Arm. CREDIT: Robert Hurt, IPAC; Bill Saxton, NRAO/AUI/NSF.

封面：银河系本地臂可能是英仙臂的一个主分支（取自美国国立射电天文台网站 http://www.nrao.edu）

Annual Report’2013－Content

I

目录

2013 年度科研工作总结 ......................................................................................... 1

2013 年度发表论文摘要 (Abstract List of Publications in 2013) ..................... 20

I. Dark Matter & Space Astronomy ............................................................... 21

Cosmology, Dark Matter and High-Energy Astrophysics ................................. 21

(1) New constraints on anisotropic rotation of CMB polarization, JCAP, 6, 1-13, Yu, Bo ... 21

(2) Contribution of ultracompact dark matter minihalos to the isotropic radio background,

physical review d, 87, 8, 083519(1)-(6), Lu, Tan ............................................................. 21

(3) Impact of the local void on the cosmological parameters, JCAP, 3, 1-18, Yu, Bo* ........ 21

(4) The relation between pauli and gamma representation in qed(3) and induced chern-simons

term, chinese science bulletin ,58,31,3735-3737, Sun Wei-Min ............................................ 21

Gamma-Ray Burst, Neutron Star and relevant physics .................................... 22

(5) Dust extinctions for an unbiased sample of gamma-ray burst afterglows, MNRAS, 432,

2, 1231-1244, Jin, Zhi-Ping ......................................................................................... 22

(6) GRB 081007 and GRB 090424: The surrounding medium, outflows, and supernovae,

ApJ, 774, 2, 114 (1) - (9) , Jin, Zhi-Ping* ........................................................................ 22

(7) The last three outbursts of H1743-322 observed by RXTE in its latest service

phase, MNRAS, 431, 3, 2285-2293, Zhou, Jia-Neng* ............................................ 23

(8) Is the late near-infrared bump in short-hard grb 130603b due to the li-paczynski

kilonova?, ApJL,775, 1, L19(1)-(4), Jin, Zhi-Ping*.......................................................... 23

(9) Cosmological Time Dilation in Durations of Swift Long Gamma-Ray Bursts, ApJL, 778,

1, L11(1)-(5), Zhang, Fu-Wen* ..................................................................................... 23

(10) Multi-wavelength Study of the Be/X-ray Binaries, IAU Symposium, 290, 351-352, Yan,

Jing-Zhi* ................................................................................................................... 24

High-Energy Solar Astrophysics ......................................................................... 24

(11) 2D and 3D Polar Plume Analysis from the Three Vantage Positions of STEREO/EUVI

A, B, and SOHO/EIT, solar physics, 283, 1, 207-225, Feng, Li ......................................... 24

(12) Observations of a Quasi-periodic, Fast-Propagating Magnetosonic Wave in Multiple

Wavelengths and Its Interaction with Other Magnetic Structures, solar physics, 288, 2, 585-602,

Li, Hui ...................................................................................................................... 24

(13) Electron and proton acceleration during the first ground level enhancement event of solar

cycle 24, ApJ, 770, 1, 34(1)-(11), Firoz, Kazi A. .............................................................. 25

(14) Imaging coronal magnetic-field reconnection in a solar flare, nature physics,

9, 8, 489-493, Su, Yang* .......................................................................................... 25

(15) Error Assessment in Modeling with Fractal Brownian Motions, fractals, 21, 4,

1-6, Qiao, Bing-Qiang* ........................................................................................... 25

(16) The breakdown of the power-law frequency distributions for the hard X-ray

peak count rates of solar flares, RAA, 13, 12, 1482-1492, Li, You-Ping* ............... 26

(17) Comparisons of CME Morphological Characteristics Derived from Five 3D

Reconstruction Methods, solar physics, 282, 1,221-238, Feng, Li*........................ 26

(18) High-z quasars in the r-h = ct universe,ApJ,764, 1,72(1)-(5), Melia, Fulvio* .................. 26

(19) Energy partition between energetic electrons and turbulent magnetic field in

supernova remnant rx j1713.7-3946, ApJ,773,2,138(1)-(6), Yang, Chu-Yuan* ...... 27 (20) Magnetic energy partition between the coronal mass ejection and flare from

AR 11283, ApJ,765, 1,37(1)-(11), Feng, Li* .......................................................... 27

(21) Kelvin-helmholtz instability of a coronal streamer, ApJ, 774, 2, 141(1)-(9),

Feng, Li* ................................................................................................................. 27

(22) Impulsive Thermal X-Ray Emission from a Low-lying Coronal Loop,ApJ,

769, 2, 135(1)-(10), Liu, Si-Ming* .......................................................................... 28

PMO

中国科学院紫金山天文台

科技处地址：南京市北京西路 2 号

邮编：210008

电话：+86-25-8333-2288, 2018

传真：+86-25-8333-2288

电邮：[email protected]

http://www.pmo.cas.cn

编委

熊大闰陆埮

杨戟鲁春林甘为群

赵长印常进史生才马月华

韦大明季海生冯珑珑康熙

高煜王红池徐烨徐劲

姚大志傅燕宁吴德金徐伟彪

季江徽赵海斌

文字编辑

朱留斌 [email protected]

李琳 [email protected]

责任编辑

毛瑞青 [email protected] 注：目录中文章作者只列排名最前的本单位人员，作者名后带*者为第一作者文章，

未带星号者为非第一作者文章。

mailto:[email protected]

http://www.pmo.cas.cn/




Purple Mountain Observatory CAS

II

(23) Parameters of the flare and surrounding medium and their evolution during

20 January 2005 solar event, JPCS, 409, 1, 012204(1)-(9), Gan, Wei-Qun ............ 28

(24) Polar jet kinetics and energetics analysed from STEREO/COR data, IAU

Symposium, 294,549-550, Feng, Li* ...................................................................... 28

(25) Solar Flares with an Exponential Growth of the Emission Measure in the Impulsive

Phase Derived from X-ray Observations,CAA,37,3,277-293,Han, Fei-Ran* ...................... 29

(26) A Research on CdZnTe Array Detector,AcASn,54,5,467-477,Cai Ming-Sheng* ........ 29

Multi-Band Observation of Solar Activity .......................................................... 29

(27) Ha Surges Aroused by Newly-emerging Satellite Bipolar Magnetic Field,

AcASn, 54, 4,318-326, Zhou, Tuan-hui .................................................................. 29

(28) Recent advances in solar storm studies in China, science china-earth sciences,

56, 7,1091-1117, Ji Hai-Sheng ............................................................................... 30

(29) Spatially Resolved Microwave Observations of Multiple Periodicities in a Flaring Loop,

solar physics,284, 2,559-578, Melnikov, V. F. .................................................................. 30

(30) Parametric survey of longitudinal prominence oscillation simulations, A&A,

554, A124(1)-(8), Zhang, Qing-Min* ...................................................................... 30

(31) Observation of magnetic reconnection driven by granular scale advection, ApJL, 769, 2,

L33(1)-(7), Ji, Hai-Sheng ............................................................................................ 31

(32) Concerning spikes in emission and absorption in the microwave range, RAA,

13, 1, 115-128, Huang, Guang-Li ........................................................................... 31

(33) The calculation of coronal magnetic field and density of nonthermal electrons in the

2003 October 27 microwave burst,RAA,13,2,215-225,Huang, Guang-Li* ........................ 32

(34) Analysis of the coronal source of the partially limb-occulted flare on 2002 July 20,

RAA,13, 8, 961-977, Shen, Jin-Hua* ............................................................................ 32

(35) The contracting and unshearing motion of flare loops in the X 7.1 flare on 2005 January

20 during its rising phase,RAA,13,5,526-536,Zhou, Tuan-Hui* ........................................ 32

(36) Statistical study of UV bright points and magnetic elements from SDO observations,

new astronomy, 23-24, 19-26, Li, Dong* ....................................................................... 33

(37) Determination of intrinsic mode and linear mode coupling in solar microwave

bursts, IJASS, 345, 1,41-47, Huang, Guang-Li* ..................................................... 33

(38) Frequency dependence of solar flare occurrence rates-inferred from power-law

distribution, IJASS,347,1,15-19, Song, Qi-Wu* ............................................................... 34

(39) X-ray source motion along the loop in two solar flares, IJASS,346,2, 307-318,

Ning, Zong-Jun* ...................................................................................................... 34

(40) Chromospheric evaporation in sympathetic coronal bright points, A&A,557,

L5(1)-(4), Zhang, Qing-Min* .................................................................................. 34

(41) Double power-law distribution of magnetic energy in the solar corona over an

active region, ApJ,764,1,86(1)-(9), Shen, Jin-Hua* ................................................ 35

Laboratory for Dark Matter and Space Astronomy .......................................... 35

(42) First-Principle of the Electronic Structure and Optical Property of LaBr_3 Under High

Pressure, acta optica sinica, 33, 2, 216002(1)-(8), Ma, Tao ............................................... 35

(43) Gamma-ray Spectrometer onboard Chang'E-2, nucl instrum meth a,726,

113-115, Ma, Tao* ................................................................................................... 35

(44) The Method to Get Background for Chang'E-1 GRS, AcASn,54,4,262-369, Ma, Tao* 36

(45) Fermi/LAT observations of GRB 110625A, EAS Publications Series,61,

83-85, Fan, Yi.-Zhong ............................................................................................. 36

(46) Upturn observed in heavy nuclei to iron ratios by the ATIC-2 experiment, 23rd European

Cosmic Ray Symposium,56,284-289, Chang, Jin. .......................................................... 36 (47) Potassium Map from Chang' E-2 Constraints the Impact of Crisium and Orientale Basin

on the Moon, scientific reports, 3, 1611 (1) - (6), Chang, Jin ............................................. 36

(48) A hybrid model of GeV-TeV gamma ray emission from the Galactic center, j phys g

nucl partic, 40, 6, 65201(1)-(9), Yuan, Qiang .................................................................. 37 (49) Theoretical study on neutron skin thickness of Ca isotopes by parity-violating electron

scattering, nuclear physics a, 900, 1-15, Dong, Tie-Kuang................................................ 37

PMO

Purple Mountain Observatory

Chinese Academy of Sciences

ADD：2 West Beijing Road,

Nanjing 210008, China

TEL： +86-25-83332288

FAX： +86-25-83332288

Email：[email protected]

http://www.pmo.cas.cn

Editor Commettee

Darun XIONG, Tan LU

Ji YANG, Chunlin LU, Weiqun GAN

Zhangyin ZHAO, Jin CHAN,

Sheng-Cai SHI, Yuehua MA,

Daming WEI, Haisheng JI,

Longlong FENG, Xi KANG, Yu GAO,

Hongchi WANG, Ye XU, Jin Xu,

Dazhi YAO, Yanning FU, Weibiao

XU, Jianghui JI, Haibin ZHAO

Sub-Editor

Liubin ZHU [email protected]

Lin LI [email protected]

Excutive Editor

Rui-Qing MAO [email protected]

Division of

Science & Technology Management


http://www.pmo.cas.cn/





III

(50) Constraints on the dark matter annihilation scenario of Fermi 130 GeV gamma-ray line emission by continuous

gamma-rays, Milky Way halo, galaxy clusters and dwarf galaxies observations, journal of cosmology and astroparticle physics,

5, E02-1, Yuan, Qiang .............................................................................................................................................. 37

(51) A generic method to constrain the dark matter model parameters from Fermi observations of dwarf

spheroids, journal of cosmology and astroparticle physics, 3, 18(1)-(14), Yuan, Qiang ..................................... 38

(52) Dissecting X-ray-Emitting Gas Around the Center of Our Galaxy,science,341,6149,981-983,Ji, Li ....... 38

(53) Nuclear charge radii of heavy and superheavy nuclei from the experimental alpha-decay energies and

half-lives, physical review c, 87, 224310(1)-(9), Dong, Tie-Kuang .................................................................... 38

(54) The narrow x-ray tail and double H alpha tails of ESO 137-002 in A3627, ApJ, 777, 2, 122(1)-(13), Ji, Li ................ 39

(55) Gamma-ray Spectrometer onboard Chang'E-2, acta astronomica sinica, 54, 3, 291-299, Ma, Tao* ......... 39

(56) PAMELA/Fermi-LAT electron cosmic ray spectrum at similar to 100 GeV: Implication for dark matter annihilation

signal in accordance with the 130 GeV gamma-ray line, physics letters b,720,39540(1)-(5), Feng, Lei* ............................... 39

(57) Diffuse PeV neutrino emission from ultraluminous infrared galaxies, physical review d,87,6, 63011(1)-(5), He,

Hao-Ning*.............................................................................................................................................................. 40

(58) Signature of gravitational wave radiation in afterglows of short gamma-ray bursts?, physical review d,

88, 6, 67304(1)-(4), Fan, Yi-Zhong* .................................................................................................................... 40

(59) Decaying asymmetric dark matter relaxes the AMS-Fermi tension, journal of cosmology and

astroparticle physics,10,8,1-15, Feng, Lei* .......................................................................................................... 40

(60) A Supramassive Magnetar Central Engine for GRB 130603B, ApJL,779,2,L25(1)-(4),Fan, Yi-Zhong* . 40

(61) High-energy emission of GRB 130427A: Evidence for inverse compton radiation, ApJ, 776, 2, 95(1)-(9),

Fan, Yi-Zhong* ..................................................................................................................................................... 41

(62) Constraining the distribution of dark matter in the inner galaxy with an indirect detection signal: the case of a tentative

130 gev gamma-ray line, ApJ,770,2,127(1)-(5), Yang, Rui-Zhi* ..................................................................................... 41

(63) Reconcile the ams-02 positron fraction and fermi-lat/hess total e(+/-) spectra by the primary electron spectrum

hardening,727,1-3,1-7, Yuan, Qiang* ......................................................................................................................... 42

(64) Evidence for a second component in the high-energy core emission from centaurus a?,APJL,770,1,l6(1-5), Yang,

Rui-Zhi. ................................................................................................................................................................. 42

II. Antarctic Astronomy Radio Astronomy ............................................................................................... 43

Stellar Structure, Evolution and Pulsation ...................................................................................................... 43

(65) Notes on the CCD Flatfields of the YFOSC on the 2.4m Reflector of the Yunnan Observatory, astronomical research

and technology,10,3,283-287, Zhang Chun-Sheng ....................................................................................................... 43

(66) A Theoretical Probe for Excitation Mechanism of Solar-like and Mira-like Oscillations of Stars, AcASn,

54,1,20-25, Xiong Da-Run* ................................................................................................................................. 43

(67) Seismic study of solar convection and overshooting: results of nonlocal convection,RAA,13,9,

1127-1140, Deng, Li-Cai ..................................................................................................................................... 43

(68) Solar-like and Mira-like oscillations of stars - A uniform excitation mechanism, RAA, 13, 11, 1269-1294,

Xiong, Da-Run* .................................................................................................................................................... 43

(69) Are there Pulsationally Unstable Low-degree p1 Modes in the Sun, CAA, 37, 3, 294-301, Xiong,

Da-Run* ............................................................................................................................................................... 44

(70) A theoretical Probe for Excitation Mechanisms of Sun-like and Mira-like Oscillations of Stars, CAA, 37,

1, 1-7, Xiong, Da-Run* ........................................................................................................................................ 44

Center for Antarctic Astronomy ....................................................................................................................... 44

(71) The simulation techniques and applications in modern cosmology, SCIENCE SINICA Physica,

Mechanica & Astronomica,43,6,687-707, Feng, Long-Long* ............................................................................. 44

(72) Turbulence effect of the intergalactic medium, AcASn, 54, 4, 401-402, Zhu, Wei-Shan* ......................... 45

(73) Gravitational lensing effects on submillimetre galaxy counts,MNRAS,430,2,1423-1432, Li, Guo-Liang...................... 45

(74) The mass profile and accretion history of cold dark matter haloes, MNRAS , 432, 2, 1103-1113, Li, Ming ................ 45

(75) A Complete Reference of the Analytical Synchrotron External Shock Models of Gamma-Ray Bursts,

New Astronomy Reviews,57,5,141-190, Gao, He* ............................................................................................. 46

(76) Peculiar velocity decomposition, redshift space distortion, and velocity reconstruction in redshift surveys:

The methodology, physical review d, 87, 6, 063526(1)-(17), Pan, Jun ............................................................... 46

(77) Compton scattering of self-absorbed synchrotron emission, MNRAS, 435, 3, 2520-2531, Gao, He* ..... 47

(78) Interpretation of the unprecedentedly long-lived high-energy emission of GRB 130427A,ApJL,773,2,

L20(1)-(5), Wu, Xue-Feng ................................................................................................................................... 47

(79) Multipole gravitational lensing and high-order perturbations on the quadrupole lens,ApJ,765,2,

134(1)-(10), Kang, Xi .......................................................................................................................................... 48


IV

(80) Early afterglows of gamma-ray bursts in a stratified medium with a power-law density distribution, ApJ,

776, 2, 120(1)-(15), Wu, Xue-Feng ...................................................................................................................... 48

(81) Delayed energy injection model for gamma-ray burst afterglows, ApJ, 779, 1, 28(1)-(20), Wu,

Xue-Feng ............................................................................................................................................................. 48

(82) Turbulence in the intergalactic medium: solenoidal and dilatational motions and the impact of numerical

viscosity, ApJ, 777, 1, 48(1)-(17), Zhu, Wei-Shan* .............................................................................................. 49

(83) Evidence for Two Distinct Populations of Type Ia Supernovaee, science, 340, 6129, 170-173, Wang, Li-Fan ............ 49

(84) Image analysis for cosmology: results from the great10 star challenge,ApJS,205,2,12(1)-(11), Li, Guo-Liang ........... 49

(85) Possible high-energy neutrino and photon signals from gravitational wave bursts due to double neutron

star mergers, physical review d, 88, 4, 43010(1)-(6), Gao, He* .......................................................................... 50

(86) A comprehensive study of gamma-ray burst optical emission. II. Afterglow onset and late re-brightening

components, ApJ, 774, 1, 13(1)-(16), Gao, He .................................................................................................... 50

(87) Further evidence for the accretion disc origination of the double-peaked broad H alpha of 3C 390.3,

MNRAS, 431, 1, L112-L116, Zhang, Xue-Guang* ............................................................................................. 51

(88) Optical spectral index-luminosity relation for the 17 mapped Palomar-Green quasars, MNRAS, 435, 3,

2141-2151, Zhang, Xue-Guang* .......................................................................................................................... 51

(89) More evidence for the intermediate broad line region of the mapped AGN PG 0052+251, MNRAS, 434,

3, 2664-2678, Zhang, Xue-Guang* ...................................................................................................................... 51

(90) Correlation between the line width and the line flux of the double-peaked broad H alpha of 3C390.3,

MNRAS, 429, 3, 2274-2286, Zhang, Xue-Guang* .............................................................................................. 52

(91) Giant X-ray bump in GRB 121027A: evidence for fall-back disk accretion, ApJL, 767, 2, L36(1)-(5), Wu,

Xue-Feng* ............................................................................................................................................................ 52

(92) The Gamma-Ray Burst Hubble Diagram and Its Implications for Cosmology, ApJ, 772, 1, 43(1)-(11),

Wu, Xue-Feng ...................................................................................................................................................... 52

(93) Bright Broadband Afterglows of Gravitational Wave Bursts from Mergers of Binary Neutron Stars, ApJ,

771, 2, 86(1)-(8), Gao, He* .................................................................................................................................. 53

(94) Is There a Relation between Duration and Eiso in Gamma-Ray Bursts?, IAU Symposium, 290, 1,

223-224, Wu, Xue-Feng ....................................................................................................................................... 53

(95) Shape measurement by using basis functions, IAU Symposium, 288, 306-308, Li, Guo-Liang* ............. 53

(96) Photometry of variable stars from Dome A, antarctica: results from the 2010 observing season, AJ, 146,

6, 1-14, Wang, Li-Fan .......................................................................................................................................... 54

(97) Discovery Of An Extra Hard Spectral Component In The High-Energy Afterglow Emission Of GRB

130427A, 771,1,L13(1-5), Hou, Shu-Jin ............................................................................................................. 54

Galaxy Cosmology and Dark Energy............................................................................................................... 54

(98) The dependence of tidal stripping efficiency on the satellite and host galaxy morphology,MNRAS,431,4,

3533-3542, Chang, Jiang* ................................................................................................................................... 54

(99) The effect of warm dark matter on galaxy properties: constraints from the stellar mass function and the

tully-fisher relation, ApJ,767,1,22(1)-(7), Kang, Xi* ........................................................................................... 55

(100) Alignments Of Galaxies Within Cosmic Filaments From SDSS DR7,ApJ,779,2,160(1-10), Wang, Lei ................... 55

Star Formation in Galaxies ....................................................................................................................... 56

(101) A Herschel Spectroscopic Survey of Warm Molecular Gas in Local Luminous Infrared Galaxies,ASPC,

477,31-35, Gao, Yu .............................................................................................................................................. 56

(102) The Star Formation Efficiency in Stephan's Quintet Intragroup Regions, Conference Proceedings

"galaxy Mergers In An Evolving Universe",477,73-76, Gao, Yu ........................................................................ 56

(103) The nature of [S III]lambda lambda 9096, 9532 emitters at z=1.34 and 1.23, science china-physics

mechanics & astronomy, 56, 11, 2226-2235, Zheng Xian-Zhong ........................................................................ 56

(104) H2O emission in high-z ultra-luminous infrared galaxies, A&A, 551, A115(1)-(12), Gao, Yu ................. 57

(105) Water vapor in nearby infrared galaxies as probed by herschel, ApJL,771, 2, L24(1)-(6), Gao, Yu ......... 57

(106) A SiO 2-1 survey toward gas-rich active galaxies, ApJL, 778, 2, L39(1)-(5), Zhang, Zhi-Yu .................. 57

(107) High resolution observations of the 6 cm H2CO maser in NGC 6240, RAA,13,3,270-276, Zhang, Zhi-Yu ............... 58

(108) Shock-enhanced C+ emission and the detection of H2O from the stephan's quintet group-wide shock

using herschel, ApJ,777,1,66(1)-(16), Gao, Yu .................................................................................................... 58

(109) Evidence for CO Shock Excitation in NGC 6240 from Herschel SPIRE Spectroscopy,ApJL,762,2,

L16(1)-(5), Gao, Yu ............................................................................................................................................. 58

(110) Multi-wavelength study of a complete irac 3.6 mu m selected galaxy sample: a fair census of red and

blue populations at redshifts 0.4-1.2, ApJ,766,1,21(1)-(17), Zheng, Xian-Zhong ............................................... 59

(111) AGN host galaxies at redshift z ≈ 0.7: peculiar or not?, A&A,549,1,46-61, Zheng, Xian-zhong ......... 59


V

(112) A deep search for molecular gas in two massive lyman break galaxies at z=3 and 4: vanishing

co-emission due to low metallicity?, ApJL,776,2,L24(1)-(6), Gao, Yu ............................................................... 60

(113) A herschel survey of the [N II] 205 mu m line in local luminous infrared galaxies: the [N II] 205 mu m

emission as a star formation rate indicator, ApJL,765,1,L13(1)-(6), Zhao, Ying-He* .......................................... 60

(114) The Intrinsic Scatter Along The Main Sequence of Star-Forming Galaxies at z ~ 0.7,ApJ,778,1, 23(1)-(9),

Guo, Ke-Xin* ........................................................................................................................................................ 60

(115) A Study on the Chemical Properties of Blue Compact Dwarf Galaxies,ApJ,764,1,44(1)-(11), Zhao,

Ying-He* ............................................................................................................................................................... 61

(116) Looking for molecular gas in a massive lyman break galaxy at z = 4.05, IAU Symposium,259,1,23, Tan,

Qing-Hua*............................................................................................................................................................ 61

(117) A Herschel Survey of the [NII] 205 micron Emission in Local Infrared Luminous Galaxies, IAU

Symposium,292,1,256, Zhao, Ying-He* ............................................................................................................... 61

(118) The Co-Evolution of Supermassive Black Holes and Galaxies: Observational Constraints,ApJ,295,

109-116, Zheng, Xian-Zhong* .............................................................................................................................. 61

(119) Muscle w49: a multi-scale continuum and line exploration of the most luminous star formation region in the milky way.

i. data and the mass structure of the giant molecular cloud, ApJ,779,2,121(1-28), Zhang, Zhi-Yu ........................................ 62

Molecular Clouds and Star Formation ............................................................................................................ 62

(120) A Study on the Molecular Lines of CO Isotopes in the Star Forming Region AFGL 5157, AcASn,54,4,

305-317, Yang, Ji ................................................................................................................................................. 62

(121) Study on Description Methods of Mass Segregation of Star Clusters, progress in astronomy,31,2,

202-212, Er, Xin-Yue* .......................................................................................................................................... 63

(122) Mass segregation of embedded clusters in the Milky Way, RAA, 13, 3, 277-289, Er, Xin-Yue* ............... 63

(123) Hα emission objects in Circinus, astronomische nachrichten,334,3,282-287, Chen, Zhi-Wei .................. 63

(124) The thermal state of molecular clouds in the Galactic center: Evidence for non-photon-driven heating,

A&A,550, A135(1)-(18), Ao, Yi-Ping* ................................................................................................................ 64

(125) Young stars in epsilon Chamaleontis and their disks: disk evolution in sparse associations, A&A, 549,

A15(1)-(17), Fang, Min* ..................................................................................................................................... 64

(126) Star-forming regions of the Aquila rift cloud complex I. NH3 tracers of dense molecular cores,A&A,

553, A58(1)-(25), Wang, Min............................................................................................................................... 65

(127) OTS 44: Disk and accretion at the planetary border, A&A,558, L7(1)-(5), Liu, Yao ................................ 65

(128) Refined physical properties and g', r', i', z', J, H, K transmission spectrum of WASP-23b from the ground,

A&A,553, A26(1)-(8), Chen, Guo ....................................................................................................................... 66

(129) The link between magnetic fields and filamentary clouds: bimodal cloud orientations in the Gould Belt,

MNRAS,436,4,3707-3719, Fang, Min ................................................................................................................ 66

(130) Physical properties, transmission and emission spectra of the WASP-19 planetary system from

multi-colour photometry,MNRAS,436,1,2-18, Chen, Guo .................................................................................. 66

(131) High-precision photometry by telescope defocusing– V. WASP-15 and WASP-16,MNRAS,434,3,

1300-1308, Chen, Guo......................................................................................................................................... 67

(132) Photometry of variable stars from dome a, antarctica: results from the 2010 observing season, AJ, 146, 6,

139(1)-(10), Yang, Ji ............................................................................................................................................ 67

(133) Ground-based Detections of Thermal Emission from the Dense Hot Jupiter WASP-43b in the H and Ks

Bands,ApJ,770,1,70(1)-(8), Chen, Guo ............................................................................................................... 68

(134) AFGL 5157 NH3: a new stellar cluster in the forming process,RAA,13,6,695-704, Jiang, Zhi-Bo* ....... 68

(135) CO observations of the Galactic bubble N4,RAA,13,8,921-934, Li, Jun-Yu* ........................................... 68

(136) A comparison of approaches in fitting continuum SEDs,RAA,13,4,420-434, Liu, Yao* .......................... 69

(137) Radiative transfer modeling of three T Tauri stars: selecting candidates for studying circumstellar disk

evolution,RAA,13,7,841-848, Liu, Yao* .............................................................................................................. 69

(138) Conceptual design studies of the 5m terahertz antenna for Dome A, Antarctica, RAA, 13, 12, 1493-1508,

Yang, Ji ................................................................................................................................................................ 69

(139) CEN 34-high-mass YSO in M 17 or background post-AGB star?,A&A,557,1,A51-A59, Chen, Zhi-Wei* ................ 70

(140) Proper motions of molecular hydrogen outflows in the rho Ophiuchi molecular cloud,A&A,553,A41,

A41(1)-(37), Wang, Hong-Chi ............................................................................................................................. 70

(141) SMA observations of class 0 protostars: a high angular resolution survey of protostellar binary systems,

ApJ,768,2,110(1)-(31), Chen, Xue-Peng* ............................................................................................................ 71

(142) Young stellar objects in lynds 1641: disks, accretion, and star formation history,ApJS,207,1,5(1)-(39), Fang, Min* .... 72

(143) Unveiling the Physical Properties and Kinematics of Molecular Gas in the Antennae Galaxies with the

SMA, ASP Conference Proceedings,477,1,311-312, Mao, Rui-Qing .................................................................. 72

(144) Molecular Gas Around the Infrared Dust Bubbles, IAU Symposium,292,1,43, Gong, Yan* .................... 72


VI

(145) Triggered Star Formation at the End of the Galactic Bar?, Protostars and Planets VI , Gong, Yan* ......... 73

(146) Gradients Of Stellar Population Properties And Evolution Clues In A Nearby Galaxy M101,

769,2,127(1-13), Mao, Ye-Wei ............................................................................................................................. 73

(147) Initial Considerations of the 5 Meter Dome A Terahertz Explorer (DATE5) for Antarctica,ISAP, 1,21-24, Yang, Ji* ... 73

Laboratory for Millimeter & Sub-Millimeter Wave ....................................................................................... 73

(148) Design of Bandpass Filters Using Three Parallel Coupled-Lines with Open Stub Resonator, chinese

journal of electronics, 22, 1, 192-194, Yang, Jin-Ping ......................................................................................... 73

(149) Development of a Dual Polarization SIS Mixer With a Planar Orthomode Transducer at 350 GHz, ieee

transactions on applied superconductivity, 23, 3, 1400705(1)-(5), Shi, Sheng-Cai ............................................. 74

(150) The influence of CeO2 nano-dots decoration on substrates on flux pinning strength in Tl2Ba2CaCu2O8

thin films, ieee transactions on applied superconductivity, 23, 3, 8001505(1)-(5), Wang, Zheng ....................... 74

(151) Beam and phase distributions of a terahertz quantum cascade wire laser, applied physics letters, 102, 11,

111113(1)-(5), Ren, Yuan ..................................................................................................................................... 74

(152) Hot electron bolometer heterodyne receiver with a 4.7-THz quantum cascade laser as a local oscillator,

applied physics letters, 102, 1, 11123(1)-(4), Ren, Yuan ...................................................................................... 75

(153) Characterization of the IF Bandwidth of an All-NbN Superconductor-Insulator-Superconductor Mixer,

ieee transactions on applied superconductivity, 23, 3, 1400504(1)-(4), Liu Dong* ............................................. 75

(154) Direct Measurement of the Input RF Noise of Superconducting Hot Electron Bolometer Receivers, ieee

transactions on applied superconductivity, 23, 3, 2300104(1)-(4), Miao, Wei* ................................................... 75

(155) Measurement of the spectral response of spiral antenna coupled superconducting hot electron bolometers,

ieee transactions on applied superconductivity, 23, 3, 2300804(1)-(4), Zhang, Wen* ......................................... 75

(156) Phase-locking of a terahertz solid-state source using a superconducting hot-electron bolometer mixer,

superconductor science & technology, 26, 8, 85005(1)-(4), Miao, Wei* ............................................................. 76

(157) Closed-form design formulations of arbitrary phase delay crossover based on admittance matrix,

Progress in Electromagnetics Research Letters, 43, 165-173, Yang, Jin-Ping .................................................... 76

Qinhai Observation Station ...................................................................................................................... 76

(158) A double-jet system in the G31.41+0.31 hot molecular core,A&A,549,A122,A122(1)-(22), Li, Jing-Jing ................ 76

(159) On the hadronic γ-ray emission from Tycho's supernova remnant,MNRAS,429,1,L25-L29,Zhou, Xin ... 77

(160) A search for 95 GHz Class I methanol masers in molecular outflows, ApJ,763,1,2(1)-(21), Xu, Ye ........ 77

(161) Parallaxes for w49n and g048.60+0.02: distant star forming regions in the perseus spiral arm,ApJ,775,1,

79(1)-(13), Xu, Ye ................................................................................................................................................ 78

(162) On the nature of the local spiral arm of the milky way, ApJ,769,1,15 (1) - (19), Xu, Ye* ......................... 78

(163) Design study on near-field radio holography of the 5-meter dome a terahertz explorer, isap,1,25-28, Zuo, Ying-Xi* .. 78

III. Applied Celestial Mechanics and Space Object & Debris Research .................................................. 79

Center for Space Object and Debris Research ................................................................................................ 79

(164) Frequency Analysis of the Motion of Mars Orbiter Due to Nonspheric Attraction Perturbation, Journal of

Spacecraft TT & C Technology,771,86,357-362, Wang, Xin ............................................................................... 79

(165) A Method of Detecting Space Debris Based on Prior Information,AcASn,54,2,168-175,Sun, Rong-Yu* ....................... 79

(166) Scheduling Strategy for Electro-Optical Tracking of Space Objects, Journal of Spacecraft TT & C

Technology,32,1,89-94, Wang, Xin* ..................................................................................................................... 79

(167) The Bootstrap Estimation of the Accuracy of Preliminary Orbit Determination,AcASn,54,1,73-78, Wang,

Xin*

................................................................................................................................................................. 79

(168) Design and Implementation of CNEOST Image Database Based on NoSQL System,AcASn,54,4,

382-391, Wang, Xin* ............................................................................................................................................ 80

(169) A Robust Method of Preliminary Orbit Determination, AcASn,54,3,274-281, Wang, Xin* ..................... 80

(170) A Modified Gooding's Method to Calculate Inclination Function, AcASn,54,1,62-68, Wu, Lian-Da*..... 80

(171) A Method to Calculate Inclination Function with Jacobi Polynomials,AcASn,54,1,49-58,Wu,Lian-Da* ....................... 80

(172) The Comparison between Two Methods to Calculate Inclination Function with d-function,AcASn,54,2,

147-160, Wu, Lian-Da* ........................................................................................................................................ 80

(173) A Research on a Special Singularity of Recursion Formulae in Inclination Function Computation,

AcASn,54,2,161-167, Wu, Lian-Da* ................................................................................................................... 81

(174) A Quad-precision Calculation Test for Inclination Function, AcASn, 54, 3, 235-244, Wu, Lian-Da* ...... 81

(175) Stability Analysis of Recursion Relation for Inclination Function,AcASn,54,3,229-234,Wu,Lian-Da* ... 81

(176) Analysis of the applicability of collision probability algorithms for nonlinear relative motion, science

china-physics mechanics & astronomy, 56, 5, 1041-1046, Xu Xiao-Li* .............................................................. 81

(177) The unified ideal model of mean motion resonance of artificial satellites due to geopotential

perturbations, science china-physics mechanics & astronomy, 56, 4, 840-847, Zhang Ming-Jiang* .................. 82


VII

(178) Dynamical evolution of high area-to-mass ratio objects in Molniya orbits, advances in space research, 51,

11, 2136-2144, Sun, Rong-yu* ............................................................................................................................. 82

(179) Two-dimensional phase plane structure and the stability of the orbital motion for space debris in the

geosynchronous ring, advances in space research, 52, 4, 677-684, Zhao, Chang-Yin* ........................................ 82

(180) A new source extraction algorithm for optical space debris observation,RAA,13,5,604-614, Sun, Rong-Yu* .............. 83

(181) An innovative image reconstruction method for high precision astrometry, publications of the

astronomical society of japan, 65, 5, 110(1)-(9), Sun, Rong-Yu* ......................................................................... 83

(182) 北斗导航卫星同步轨道的共振特性及长期演化, 第四届中国卫星导航学术年会, 1-5, 侯永刚* ............................... 83

(183) Searching for space debris in GEO, 第七届全国空间碎片学术交流会, 1, 52-58, Sun, Rong-Yu*......... 83

(184) 加权最小二乘在精密天文定位中的应用, 第四届中国卫星导航学术年会, 孙荣煜* ............................................. 83

(185) Space Objects Photometry Using Optical Telescope Array, Space Debris Research,1,28-31, Zhang, Chen* ............... 84

(186) The long-term evolution of the plane of GEO disposal orbits, 第七届全国空间碎片学术交流会, 1, 997-1004, Zhang,

Ming-jiang* .......................................................................................................................................................... 84

IV. Planetary Sciences and Deep Space Exploration ................................................................................. 85

Near Earth Object Survey and Solar System Bodies ...................................................................................... 85

(187) Numerical simulation of time delay interferometry for a LISA-like mission with the simplification of

having only one interferometer, ASR, 51, 1, 198-206, Ni, W. -T ......................................................................... 85

Ephemerial Astronomy and Astronomical Reference System ....................................................................... 85

(188) Comparisons and Evalustions of JPL Ephemerides, AcASn, 54, 6, 550-561, Deng, Xue-Mei* ................ 85

(189) The mid-term and long-term solar quasi-periodic cycles and the possible relationship with planetary

motions, AcASn, 343, 2, 511-521, Cheng, Zhuo ................................................................................................. 85

(190) On preference of Yoshida construction over Forest-Ruth fourth-order symplectic algorithm, EPJC, 73, 6,

2413(1)-(8), Wu, Xin ............................................................................................................................................ 86

(191) f (T) gravity: effects on astronomical observations and Solar system experiments and upper bounds,

MNRAS, 433, 4, 3584-3589, Deng, Xue-Mei ..................................................................................................... 86

(192) Dynamics of spin effects of compact binaries, MNRAS, 435, 3, 2246-2255, Wu, Xin ............................. 86

(193) The effect of f(T) gravity on an interplanetary clock and its time transfer link, RAA, 13, 10, 1225-1230,

Deng, Xue-Mei* ................................................................................................................................................... 87

(194) Hipparcos photocentric orbits of 72 single-lined spectroscopic binaries,AJ,145,3,81(1)-(7), Ren, Shu-Lin* ................ 87

(195) Yukawa effects on the clock onboard a drag-free satellite,MNRAS,431,4,3236-3239,Deng, Xue-Mei* .. 87

(196) Possible Yukawa gravity effects on time transfer between the Earth and Satellites, 2013年全国时间频率

学术会议论文集, 10, 471-475, Deng, Xue-Mei* ................................................................................................ 88

(197) 美国喷气推进实验室不同版本行星历表的比较, 中国宇航学会深空探测技术专业委员会第十届学术年会论文集,

10, 233-239, Deng, Xue-Mei* .............................................................................................................................. 88

(198) Constraints on Yukawa parameters by double pulsars, Proceedings of the International Astronomical

Union, 8, 372-374, Deng, Xue-Mei* .................................................................................................................... 88

(199) Linear Stability of the n-gon Relative Equilibria of the (1+n)-Body Problem, qualitative theory of

dynamical systems ,12,1,255-271, Xu, Xing-Bo* ................................................................................................ 88

The Sun and Solar System Plasmas ................................................................................................................. 88

(200) 磁流体力学之父—阿尔文,力学与实践, 35, 6, 97-99, 李兵* ................................................................ 88

(201) Experimental Studies of Kinetic Alfven Waves, Progress in Physics, 33, 2, 57-85, Wu, De-Jin* ............. 88

(202) The Dynamics of Beam-return Current Systems in the Solar Atmosphere, Progress in Astronomy, 31, 2,

160-184, Xu, Lei* ................................................................................................................................................. 89

(203) Electron cyclotron maser emission in the coronal arch as the source of Type V bursts, ApJ, 779, 1,

83(1)-(7), Wu, De-Jin........................................................................................................................................... 89

(204) On the possibility of spontaneous generation of turbulent Alfven waves in solar plasma by heavy ions,

physics of plasmas, 20, 8, 082102, Wu, C. S.* ..................................................................................................... 90

(205) Emission of radiation induced by pervading Alfven waves, physics of plasmas,20, 3, 34503(1)-(4), Zhao,

Guo-Qing*............................................................................................................................................................ 90

(206) Nonlinear interaction and parametric instability of kinetic Alfven waves in multicomponent plasmas,

physics of plasmas, 20, 3, 32308(1)-(6), Zhao, Jin-Song* ................................................................................... 90

(207) Kinetic Alfvén wave instability driven by field-aligned currents in a low-beta plasma, JGR-Space

Physics, 118, 6, 2951-2957, Chen, Ling* ............................................................................................................. 90

(208) Anomalous resistivity in beam-return currents and hard-X ray spectra of solar flares, A&A, 550,


VIII

A63(1)-(6), Xu, Lei* ............................................................................................................................................. 91

(209) Excitation of kinetic alfven waves by density striation in magneto-plasmas, ApJ,771,1,3(1)-(7), Wu, De-Jin* ............ 91

(210) Solar type III radio bursts modulated by homochromous Alfven waves,ApJ,779,1,880-885, Zhao, Guo-Qing* ......... 91

(211) Effects of alfven waves on electron cyclotron maser emission in coronal loops and solar type i radio

storms, ApJ, 770, 1, 75(1)-(9), Zhao, Guo-Qing* ................................................................................................ 92

(212) Kinetic alfven turbulence and parallel electric fields in flare loops,ApJ,767,2,109(1)-(5), Zhao, Jin-Song* ................. 92

(213) Twist Accumulation And Topology Structure Of A Solar Magnetic Flux Rope,ApJ,779,2,157(1-13), Zhao, Jin-Song.92

(214) On the possibility of spontaneous generation of turbulent Alfven waves in solar plasma by heavy ions

(vol 20, 082102, 2013), physics of plasmas ,20,11, 119902(1-1),Wu, C. S.* ....................................................... 93

(215) Alfven Waves in the Solar Wind, Chinese Journal of Space Science,33,4,353-373, Yang Lei* ............... 93

Laboratory for Astrochemistry and Planetary Sciences ................................................................................ 93

(216) Ion Microprobe Microanalytical Techniques and their Applications in Earth Sciences, Bulletin of

Mineralogy Petrology and Geochemistry, 32, 3, 310-327, Wang Ying ................................................................ 93

(217) Petrography and Mineralogy of the Lunar Regolith Breccia Dhofar 1428, Bulletin of Mineralogy,

Petrology and Geochemistry, 32, 2, 222-230, Hsu, Wei-Biao .............................................................................. 93

(218) The water content and parental magma of the second chassignite NWA 2737: Clues from trapped melt

inclusions in olivine, MAPS, 48, 3, 474-492, Hsu, Wei-Biao .............................................................................. 94

(219) Record of S-rich vapors on asteroid 4 Vesta: Sulfurization in the Northwest Africa 2339 eucrite, GCA,

109, 1-13, Hsu, Wei-Biao ..................................................................................................................................... 94

(220) Oxygen isotope compositions of Al-rich chondrules from carbonaceous chondrites, Mineralogical

Magazine, 77, 1, 2462, Wang, Ying* .................................................................................................................... 94

(221) SIMS dating of eucritic zircons, 76th Annual Meeting of the Meteoritical Society,48,A172, Hsu, Wei-Biao* ............. 95

(222) Youxi, a newly found mesosiderite from China, MAPS, 48, A171, Hsu, Wei-Biao* ................................ 95

(223) 富集型玄武质火星陨石 NWA 2975 的岩石学和稀土元素地球化学特征,中国矿物岩石地球化学学会

第 14 届学术年会, 19, 611-612, 徐伟彪 ........................................................................................................... 95

(224) 灶神星表面流体-岩石相互作用的陨石学记录,中国矿物岩石地球化学学会第 14 届学术年会,19, 628-629,

徐伟彪 ................................................................................................................................................................. 95

(225) 新近发现的罗布泊陨石, 中国矿物岩石地球化学学会第14届学术年会, 19, 613-614, 李少林* ................................ 95

(226) Water content and chlorine isotope composition of the moon, 第十届全国同位素地质年代学与同位素地球化学学术讨

论会论文集, 1, 1, Wang, Ying* ............................................................................................................................ 95

(227) Ion microprobe dating of zircon and baddeleyite from eucrites, 中国极地科学年会论文集, 1, 1, Wang, Ying* ......... 96

Xuyi Observation Station ...................................................................................................................... 96

(228) Observation Plan for Refining Shape Model of (6) HEBE,earth moon and planets,110,81-89, Zhao, Hai-Bin ........... 96

(229) A fast ellipsoid model for asteroids inverted from lightcurves,RAA,13,4,471-478,Zhao, Hai-Bin .......... 96

(230) Atmospheric extinction coefficients and night sky brightness at the Xuyi Observation Station, RAA, 13,

4, 490-500, Zhao, Hai-Bin ................................................................................................................................... 96

(231) Photometric Observation of 1542 Schalen, Minor Planet Bulletin, 40, 2, 68-69, Li, Bin* ........................ 97

(232) Lightcurve Analysis of Four Asteroids, Minor Planet Bulletin, 40, 2, 62-63, Li, Bin* ............................. 97

(233) Photometric Observation of 3024 Hainan, 3920 Aubignan, and 5951 Alicemonet, Minor Planet Bulletin,

40, 1, 43-44, Li, Bin* ............................................................................................................................................ 97

Laboratory for Planetary Science and Deep Space Exploration ................................................................... 97

(234) 嫦娥二号卫星多目标多任务设计与经验,中国科学:技术科学, 43, 6, 585-595, 季江徽 ..................... 97

(235) Tidal Evolution of the Kepler Candidate Two-planet Systems, AcASn, 54, 4, 350-361, Dong, Yao* ....... 98

(236) A Study on the Characteristics of the Structure of Vega's Debris Disk,AcASn,54,2,131-146,Lu, Tao* ... 98

(237) The Review of Thermal Models for Asteroids, Progress in Astronomy,31,2,185-201,Yu, Liang-Liang* .. 98

(238) 嫦娥二号飞越小行星试验中图塔蒂斯轨道确定与精度分析,Scientia Sinica Technologica,43,5, 506-511, 胡寿村* .... 99

(239) Error Analysis and Trajectory Correction Maneuvers of Lunar Transfer Orbit,AcASn,54,3,261-273, Zhao, Yu-Hui* .. 99

(240) A Research on Imaging Strategy and Imaging Simulation of Toutatis in the Chang'e 2 Flyby Mission,

AcASn, 54, 5, 447-454, Zhao, Yu-Hui* ................................................................................................................ 99

(241) On Nominal Formation Flying Orbit with a Small Solar System Body, LNEE,187,26,391-399, Zhao, Yu-Hui* ......... 99

(242) Possible transit timing variations of the tres-3 planetary system, AJ, 145, 3, 68(1)-(8), Ji, Jiang-Hui ..... 99

(243) Tidal evolution of the Kepler-10 system, MNRAS, 430, 2, 951-960, Dong, Yao* .................................. 100

(244) Establish and use of the numerical ephmerides for Near-Earth Asteroids,第二届航天飞行动力学技术研

讨会论文集, 1, 1, Hu, Shou-Cun* ..................................................................................................................... 100


IX

(245) Using finite element definitions to compute the gravitation of Toutatis,中国宇航学会深空探测技术专

业委员会第九届学术年会论文集, 9, 111-116, Zhao, Yu-Hui* ........................................................................ 100

(246) The Ginger-shaped Asteroid 4179 Toutatis: New Observations from a Successful Flyby of Chang'e-2,

Scientific Reports, 3, 1, 3411-3416, Ji Jiang-Hui ............................................................................................. 100

(247) Investigation of Thermal Inertia and Surface Properties for Near-earth Asteroid (162173) 1999 JU3,

AcASn,54,6,537-549, Yu Liang-Liang* ............................................................................................................ 101

紫台历年发表论文情况 ................................................................................................................................... 102

专利 ................................................................................................................................................................... 102

紫台主要科研项目统计 ................................................................................................................................... 104

学术报告 ........................................................................................................................................................... 105

Annual Research Report’2013

1

2013 年度科研工作总结

一、科研工作总体情况

1. 概述

2013 年，紫台共有在研项目 259 项（包括新增项

目 97 项）。其中，主持国家重点基础研究发展计划（973）

项目 3 项和子项 5 项；主持（或承担）中国高技术研

究发展计划（863）项目 32 项（新增 12 项）；主持（或

承担）国家其他项目 11 项；主持（或承担）国家自

然科学基金项目 103 项（新增 42 项），其中重大项目

1 项、重点项目 6 项（新增 2 项）、主任基金项目 3

项、面上项目 31 项（新增 12 项）、杰出青年基金 2

项，承担国家自然科学基金重大科研仪器设备研制专

项 1 项；承担中科院空间科学战略先导科技专项 7 项

（新增 1 项），主持（或承担）中科院知识创新工程

重要方向项目 5 项，“百人计划”项目 5 项（新增 1

项），承担重大国际合作项目 1 项；承担江苏省自然

科学基金 11 项；横向项目 16 项（新增 8 项）。

2013 年，紫台共发表科技论文 247 篇，其中国际

合作论文 104 篇。SCI 论文 168 篇，影响因子 3.0 以

上的 114 篇，被引用 146 篇次；申请专利 5 件，其中

发明专利 5 件，申请软件著作权 4 件；专利授权数 6

件，其中发明专利 6 件。

2. 重要进展和重大成果

1）3 个重大突破

A 类先导专项项目“暗物质粒子探测卫星”项目

进展顺利，于 2013 年 4 月工程正式转初样阶段。科

学应用系统完成了系统方案设计并通过评审，已转入

系统软硬件研制。

完成国家重大科技基础设施“十二五”规划项目

——中国南极天文台项目建议书编制，并通过中科院

专家评审。联合完成第二台南极巡天望远镜 AST3-2

研制，并已开展漠河基地试观测。

空间目标与碎片观测系统二代光电阵正式投入

运行，形成了配置合理的低轨道空间目标与碎片编目

观测系统，显著增强了我院空间目标与碎片的监测能

力，为“天宫一号/神舟十号”任务提供危险目标监测

预警服务和保障。

2）5 个重点培育方向

在宇宙伽玛暴中发现引力波辐射迹象；首次观测

到耀斑磁重联的详细图像。“先进天基太阳天文台

（ASO-S）”入选“空间科学背景型号项目”；完成空

间莱曼望远镜、X 射线望远镜、地基两维光谱诊断

日冕仪等预研。

“太赫兹超导阵列成像系统”重大仪器专项项目

完成 850 微米波段超导探测器单元的设计与制备和

0.3K 低温制冷单元的研制；“银河画卷”巡天计划完

成约 700 平方度巡天；首次精确确定了银河系近域旋

臂的形态和运动学，发现它并非旋臂的一个刺，而可

能是部分旋臂或者主旋臂的一个分支。

天文定位、识别方法应用于我国首颗天基探测卫

星中，在中心指向误差较大的情况下，实现了实时天

文定位；通过建立扩展化理想共振模型，从理论上解

释了同步轨道带物体的双平动运动，以及左右单平动

不对称现象。建立了 Molniya 型轨道的双重共振模型，

得到了一个解析形式的首次积分。

完成 X 射线谱仪配套装置研制并成功登月；通过

分析嫦娥二号伽玛谱仪观测资料，提出产生月球深层

次物质的新观点；与上海天文台联合成立中科院行星

科学重点实验室；完成近地天体望远镜升级改造和天

体化学分析试验平台更新。

二、研究活动进展

I. 暗物质和空间天文研究部

宇宙学、暗物质及高能天体物理研究

围绕宇宙学、暗物质及高能天体物理等方面进行

深入的研究。对 Planck 卫星发表的微波背景辐射的数

据、AMS-02 有关宇宙射线中有关正负电子的数据、

Fermi 卫星的伽玛暴数据等进行了分析和研究，对伽

玛暴标准烛光关系的弥散和伽玛暴的红移分布对限


2

制暗能量性质的影响进行了估算，还分析了标准烛光、

重子声学振荡在限制暗能量性质的过程中产生的偏

差，此外，还在再电离、暗能量的解释、早期宇宙学、

相对论流体在宇宙学和中子星中的应用等方面进行

了探讨。

利用微波背景辐射数据限制了宇宙学 cpt 破坏的

各向异性参数，没有发现明显的各向异性 cpt 破坏；

研究可能的本地低密度区对宇宙学参数以及暗能量

参数限制的影响，100MPC 左右的本地低密度区可能

对分红移段的暗能量状态方程参数产生一定影响；对

伽玛暴标准烛光关系的弥散和伽玛暴的红移分布对

限制暗能量性质的影响进行了估算，发现在限制宇宙

学成分上，伽玛暴的较宽的红移分布能够弥补其标准

烛光关系弥散较大的缺点，给出与 Ia 型超新星相当的

限制。相应文章正在撰写中；在暗能量性质的限制上，

发现了存在于标准烛光和标准尺子等相应数据和方

法中的一种偏差，相应的工作已经接近尾声，文章在

撰写当中。

宇宙伽马暴、中子星及相关物理研究

主要进行高能爆发性天体的理论和观测研究，并

取得了一定的成果。其中一个重要研究进展：“我们

在国际上率先指出现有的短暴数据中已经存在着引

力波辐射的迹象，并预言慢转中子星的最大引力质量

约为 2.2-2.3 倍太阳质量”（Fan, Wu & Wei 2013 PRD;

Fan et al. 2013 ApJL）。

通过研究指出现有的短暴的电磁辐射中已可证

认引力波辐射信号。研究对象是“一些短暴中的持续

约 100 秒左右的平台状的 X 射线余辉辐射”而不是短

暴的瞬时辐射。黑洞和中子星合并一定会产生黑洞，

在这种情况下很难解释“平台状的 X 射线余辉辐射”。

2006 年 Gao & Fan 以及 Fan & Xu 为解释一些短暴的

奇特 X 射线余辉提出两颗中子星并合后可能形成一

颗自转周期约 1 毫秒并且具超强磁场(1E14 高斯以上)

的中子星，通常谓之为毫秒磁星。毫秒磁星的磁偶极

辐射很强，可以产生“平台状的 X 射线余辉辐射”或

其它新的辐射信号。最近 Rowlinson 等人系统的研究

了 Swift 卫星探测到的短暴 X 射线余辉，发现磁星模

型能解释约一半的事例。但是她们得到的这些磁星的

自转周期一般远大于 1 毫秒（对应的转动能远小于通

常认为的 1E52-1E53 erg），这和双中子星并合模型不

吻合；另外如此慢的自转也不足以有效抵抗引力塌缩，

导致磁星很难存活达百秒，与观测也不一致。一个可

能的解决方案是只有极小一部分磁偶极辐射的能量

转化为了多波段余辉辐射，绝大部分磁偶极辐射能量

被注入到双子星合并过程中抛射的外流物质中，这将

显著提高外流体的动能。在该情形下人们将探测到非

常明亮的外流体正向激波光学、射电余辉辐射，但绝

大部分短暴的光学、射电辐射都很弱，不支持该假设。

剩下的一种可能就是毫秒磁星的转动能主要被引力

波辐射带走，如果该磁星在垂直于自转轴方向上的椭

率达到～1%。而双中子星合并诞生的磁星内部的环向

磁场可能强达 1E17 高斯并且是各向异性的，这可以

导致～1%的椭率。基于这些依据，我们在国际上率先

指出现有的短暴数据中已经存在着引力波辐射的迹

象，并预言“慢转中子星的最大引力质量约为 2.2-2.3

倍太阳质量”，该值与现有的天文观测结果自洽(Fan,

Wu & Wei 2013 PRD)。

2013 年 6 月 3 日发生了另外一次重要的爆发性事

件 GRB 130603B。这个短时标伽玛暴的特征是晚期

光学光变中出现了一个红化的鼓包，被认为是双中子

星合并过程中抛出的富中子化外流体的进一步核合

成物质的后期衰变辐射。我们提出双中子星合并后形

成一颗毫秒磁星，磁星风能量注入到短暴的外流体中

会使正向激波的速度减速变慢，导致光学和 X 射线辐

射的光变改变。我们的模型可以很好的解释观测，但

要求正向激波的总能量是 1E51erg 左右，显著的小于

毫秒磁星的转动能～1E52erg。这个差别可以解释为

绝大部分能量被引力波带走了(Fan et al. 2013 ApJL)

本年度我们继续处理和分析一批 X 射线双星的

光学数据，研究他们短期和长期的光学变化，结合公

开的 X 射线数据，多波段地研究 X 射线双星中的各

种现象。我们在 Be/X 射线双星 X Per 中发现了长期

的光学变化，这种变化可能和它的 X 射线光变存在一

种相关性，这一结果已经投到 AJ，目前正在审稿当中。

我们还分析了另外一颗 Be/X 射线双星 LSV＋44 17

的长期光学分光和测光观测，发现了 Halpha 等值宽

度和 V 星等之间存在一个逆相关变化，这种变化可能

和 Be 星的物质喷发有关，它可以触发后续的 X 射线

爆发，这一研究结果已投 MNRAS。另外我们还研究

了黑洞 X 射线双星 H1743-322 在爆发状态的光变和能

谱特性，这一结果已经发表在 MNRAS 上。


3

太阳高能及相关物理过程研究

围绕紫台“一三五”规划内容，取得较好成绩：

“先进天基太阳天文台”（ASO-S)经过多轮竞争，年

内获得中科院空间科学先导专项背景型号立项；提出

的地基两维太阳光谱诊断日冕仪，进入基金委重大仪

器专项最后一轮评审; 与德国、意大利联合提案“太

阳高能辐射与高能粒子”，年末提交ESA-CAS征集合

作卫星计划；在太阳高能物理前沿研究方面取得系列

成果，包括首次观测到耀斑磁重联的详细图像，结果

发表在Nature Physics上。10月份成功举办了国际会议

《Energetic Particles in the Heliosphere》。

1）空间太阳探测项目和地面太阳探测项目预先

研究取得进展

“先进天基太阳天文台”（ASO-S)年内完成了概

念性阶段研究，4月通过了结题验收。之后，ASO-S

参与背景型号项目立项竞争，经过多轮评审，年内

ASO-S获得中科院空间科学先导专项背景型号立项。

ASO-S的科学目标是：同时观测太阳全日面矢量磁场、

耀斑非热辐射成像、以及日冕物质抛射的近日面传播，

研究磁场、耀斑、日冕物质抛射三者之间的关系，为

此设置了三个载荷。预期两年内完成背景型号阶段研

究，如果之后能够顺利工程立项，ASO-S将于2021年

发射。与ASO-S相互补，年末还与德国、意大利同行

合作提出了“太阳高能辐射与高能粒子”（SEEPE),

作为提案提交ESA-CAS小卫星征集。

在地面太阳探测项目预先研究方面，提出的"地

基两维太阳光谱诊断日冕仪"，在完成科学需求、初

步设计和研制方案的基础上，进行了部分关键技术试

验，6月申请了基金委重大仪器专项，进入基金委重

大仪器专项最后一轮评审，虽然没有通过，但进一步

优化设计工作仍在继续；与美国高山天文台等单位合

作，进行地基大口径日冕仪的设计，完成初步光学和

机械设计以及日冕仪本身和环境洁净度控制策略分

析，与美国高山天文台签署了新一轮地基大日冕仪合

作研制谅解备忘录。

此外，在天基莱曼阿尔法望远镜方面也开展了不

少工作，包括科学需求和任务要求，确定其科学目标

和研制方案，完成初步设计，开展杂散光抑制、高精

度稳像、超光滑镜面加工等技术试验并取得较大进展。

年内还完成了中法合作项目“太阳爆发探测小卫星A

阶段研究”（SMESE)的结题。

2）太阳磁重联、非热辐射和能量研究

展现前所未有的磁重联观测图像：Su et al.（2013）

通过一个太阳耀斑的EUV及X-ray的观测以所未有的

清晰度展现了磁场重联过程。SOD/AIA的多波段观测

显示冷的入流环及新形成的热的出流环，这一图像和

理论预期的完全相同。RHESSI的X-ray谱及像同时显

示加热至超过10MK高温等离子体也出现在预期的位

置上。这两种数据提供了产生太阳耀斑的磁场重联的

立体可视证据，证实流行的耀斑物理模型。同时，也

观测到一些新的特征，需要发展3维的磁场重联模型。

解释耀斑幂律分布的偏离：Li et al. (2013)首次引

入数据噪声来解释太阳耀斑HXR峰值计数的幂律律

频数分布曲线的低端偏离。新的模型拟合

HXRBS/SMM和BATSE/CGRO的太阳耀斑HXR峰值

计数分布显示幂律分布低端存在截断值大约是数据

噪声的3倍，这个结果表明，数据噪声以两种方式影

响太阳耀斑HXR峰值计数的频数幂律分布，一种通过

选择效应（不能低于一定噪声水平比如3s（噪声水平）

挑选事件），另一种是直接叠加在峰值数据引起峰值

数据误差。两种影响共同引起耀斑的HXR峰值计数频

数分布曲线在低段缺失下降。

详细计算耀斑能量：利用目前可用的最新数据，

Feng et al. (2013)探讨爆发事件的磁能在耀斑和日冕

物质抛射（CME）间的分配，为理解爆发事件的物理

过程提供信息。自由磁能基于SDO的HMI矢量磁图通

过非线性无力场外推获得；耀斑的能量考虑了热能，

非热能，辐射损失等，发现紫外波段的能量在所有可

计算能量中数值最大，是耀斑释放总能量的一个下限；

日冕物质抛射的能量则是基于三维情形精确计算其

动能和势能。比较发现，所研究事件，该X级耀斑和

CME消耗磁能相当。

硬X射线中热等离子体作用：Liu et al. (2013)发展

数学工具来提取复杂系统的统计特征，这些工具可以

使数值模拟和观测的比较更定量化。通过对一个耀斑

环多波段观测的详细分析，发现脉冲性的硬X射线可

以由温度快速变化的热等离子体产生，这一结果推翻

了脉冲性辐射由非热粒子产生这一传统观念，加深了

人们对等离子体加热和粒子加速过程的认识。

3）日冕中的物理现象研究

盔状冕流振荡现象: Feng et al. (2013)首次在白光

日冕的观测中发现盔状冕流由于开尔文-亥姆霍兹不


4

稳定性引起的振荡现象。发现该不稳定性可以很好的

定量解释LASCO观测到的冕流振荡特性，如振幅的增

加，冕流及其背景指数满足不稳定性发生的条件。通

过将中性电流片的不稳定性理论和LASCO冕流观测

相结合，可推测无法实测到的当地等离子体参数，如

阿尔芬速度，冕流外部物质流动速度等。

CME的三维重构:在CME的三维重构方面，Feng

et al. (2013)将2012年发展的CME区域拟合的三维重

构方法和目前存在的能够得到CME三维形态的其他

方法进行了全面的比较。发现Feng et al. (2012)提出的

方法具有普适性，三维重构结果和其他方法符合很好，

并且具有不受CME形状限制，具有更广泛的适用范围

等优点。

太阳磁场旋转特性：Huang et al. (2013, to be

submitted)利用空间卫星的数据分析行星际磁场的数

据，计算验证磁场的Parker模型, 用两颗卫星的数据，

通过进行相关性分析，找到两颗卫星先后观测到的同

一个磁场扰动现象，利用卫星空间位置的不同以及时

间间隔计算出该事件磁场的具体结构，了解整个太阳

磁场旋转的特征。文章初稿基本完成。

4）磁场等其它研究

Zhao et al. (2013, submitted)利用SDO高质量和高

分辨率观测数据，根据非线性无力场外推的日冕磁场

计算了磁场挤压因子（Q），推导了准分界面(QSL)

结构，研究了NOAA 11158活动区的磁场拓扑结构及

其时间演化，并讨论该活动区拓扑结构与耀斑的关系。

发现该活动区在大多数时间总体上呈现即使在耀斑

过程中也比较稳定的四极场的拓扑结构，包含双曲线

磁流管，这种结构与耀斑的发生没有明显的关系。但

是位于双曲线磁流管下方且在磁中性线上方的强准

分界面，在M6.6和X2.2耀斑前边的非常明显，说明其

与该活动区的高耀斑发生率有密切的关系。在X2.2耀

斑前，活动区存在一个小尺度高约400km的倒水滴结

构双曲线磁流管。该结构在耀斑后发生了明显的改变，

说明其与耀斑的发生直接相关。

离子声波是等离子体辐射机制中波波相互作用

重要的组成部分，Huang et al. (2013, submitted)用离子

模拟方法对离子声波的性质进行了细致的研究，了解

了离子声波的对哪些参数比较敏感，对等离子体辐射

机制的转换效率进行了分析，对今后研究等离子体辐

射机制的能量转换过程有一定的参考作用。

另外,对极高能中微子观测的分析表明极亮红外

星系中的巨超新星爆发造成的粒子加速有可能可以

解释有关观测。利用2维磁流体数值模拟程序研究了

壳状超新星遗迹随时间的演化，并用这一结果来解释

TeV壳状超新星遗迹RXJ1713的多波段观测。我们发

现在这类壳状超新星遗迹中，高能电子的能量密度和

磁场的能量密度几乎相等。

太阳活动的多波段观测研究

在上一个重点基金全优结题的基础之上，紧紧围

绕“多波段”和“高分辨率观测”这两个前沿主题，

我们又顺利申请到一项基金委重点项目，为本团组的

进一步发展奠定了良好的基础。围绕“高分辨率观测”，

我们成功引导了中国太阳物理界与美国大熊湖天文

台的合作，由此，一方面为中国太阳物理界争取了国

际大口径望远镜的观测时间，另一方面，我们的重点

项目的执行有了充分的时间保障。另外，季海生与国

台林刚华研究员一起申请到科技部项目，负责整理我

国太阳物理历史资料。我们发表了数篇审稿论文，一

项成果被列为国内天文2012 年度十大进展。引进一

名“百人计划”研究员。

太阳活动是空间天气源区，其核心问题是太阳活

动的触发机制和高能粒子的加速问题。在本年度中，

我们紧紧围绕这两个核心问题，着眼于太阳低层大气

在爆发式能量释放的储能及触发机制所起的作用，利

用地面和空间优质的高分辨率资料进行更加详细的

研究，从不同波段，因而从不同的方面，在以上核心

问题上取得了进展。其中的亮点工作为：我们通过

非线性无力场外推,首次发现太阳日冕磁场能谱结构

呈双幂律分布。我们进一步,拐点能量以上的能量密度

在耀斑过程中起到了关键作用。这一结果说明，太阳

活动的能量储存在太阳低层大气之中。另外重要的是，

我们以此给太阳活动区定义了一个新的参数：活动区

磁能谱指数，我们拟进一步仔细分析该参数与太阳活

动的关系，以期能将该参数纳入太阳活动区预报的参

数。

暗物质与空间天文实验室

2013 年，主要进行暗物质粒子探测卫星有效载荷

的研制工作，负责有效载荷总体即对有效载荷五个分

系统的研制协调及工作部署、中子探测器的研制、


5

BGO 量能器结构部分的研制工作。

载荷总体组织各分系统完成了载荷电性件的补

充测试，并配合卫星总体完成整星结构件力学试验。

整个有效载荷于 4 月下旬顺利转到初样阶段，开始初

样鉴定件单机的研制。初样研制阶段主要完成了以下

工作：1）单机方面，载荷总体组织各分系统（除硅

阵列探测器外）完成了各单机的详细设计和相关的评

审，使各单机按计划进行单机的生产。2）软件方面，

组织各分系统（除硅阵列探测器外）完成软件任务书、

软件需求分析和概要设计。硅阵列探测器完成软件任

务书评审。3）载荷总体组织各分系统和卫星总体确

定了载荷的环境试验规范。4）地面综合电测基本完

成了桌面联试所需的综测系统和探测器测试所需的

工装，并通过综测细则、测试覆盖性等评审。目前正

进行地面综测系统的最后测试工作。

中子探测器和 BGO 量能器结构件均于 2013 年 1

月底前交付卫星总体进行整星试验，4 月份随工程转

入初样阶段，进行相关器件投产，中子探测器于 12

月份进行初样件总装、BGO 晶体、光电倍增管等均于

11 月份全部到位，碳纤维箱体于 11 月份交付紫台，

随后进行封装及灌胶，目前相关工作仍紧锣密鼓地进

行。

嫦娥二号伽玛谱仪观测数据研究取得新的成果。

嫦娥三号于 2013 年 12 月 2 日成功发射，实验室参与

巡视器有效载荷粒子激发 X 射线谱仪研制任务。嫦娥

二号伽玛谱仪在世界上首次采用先进的溴化澜

(LaBr3)闪烁晶体作为主探测器，碘化铯(CsI)作为反符

合晶体成功抑制空间及卫星本底。嫦娥二号伽玛谱仪

的灵敏度远高于世界同类探测器,能敏感的区分月球

表面元素的细微差别,为后期的数据分析及科学研究

提供了坚实的基础。

利用空间卫星的数据分析行星际磁场的数据，计

算验证磁场的Parker 模型对研究太阳风性质是极有意

义的。研究人员用两颗卫星的数据，通过进行相关性

分析，找到两颗卫星先后观测到的同一个磁场扰动现

象，利用卫星空间位置的不同以及时间间隔计算出该

事件磁场的具体结构，了解整个太阳磁场旋转的特征。

1）利用嫦娥二号伽玛谱仪对月球表面大型撞击坑及

其周围溅射物放射性元素含量的观测，提出如下观点：

月球表面东海与危海盆地在其形成时，撞击深度应该

到达了下月壳，撞击事件可能把月球深层次的物质挖

掘了出来。2）利用 STEREO 卫星的磁场数据计算了

行星际磁场的旋转特征。

II. 南极天文和射电天文研究部

恒星结构、演化与脉动研究

以星震学研究为主线。参与了星震学国际合作项

目 SONG 的大部分科学讨论会，提供理论咨询。研究

工作集中在恒星的类太阳振荡和类长周期变星振荡

激发机制的探讨。

1）对近几年来的工作进行了清理和整理。多年

来随着研究工作的发展，计算程序经过不断的修改，

变得有些杂乱，今年以来较多时间，对恒星对流包层

模型计算程序和恒星非绝热脉动计算程序进行了清

理和整理，为以后研究工作打造一个较好的基础。

2）发展和完善了非各向同性对流理论下计算恒

星对流包层平衡结构以及径向和非径向脉动的程序，

并用它计算了 M=0.6―3.0M⊙恒星演化模型对流包层

结构和非绝热脉动，研究了湍动对流的非各向同性对

恒星脉动稳定性的影响。

3）研究了恒星对流包层氦丰度对恒星脉动稳定

性的影响。研究了δScuti 变星脉动不稳定区中非变星

成因的氦弥散之说。我们的结果氦弥散不太像能用来

解释δScuti 变星脉动不稳定带中的非变星。

南极天文中心

在漠河建立了南极天文设备测试极地。第二台南

极巡天望远镜 AST-2 研制完成，并且在漠河测试运行,

性能改进中。首台南极巡天望远镜 AST-1 在南极遥控

运行 50 多天。

5 月 26-29 日南极天文中心在云南组织了“2013

International Collaboration Meeting on Antarctic Survey

Telescopes”国际会议，8 月在西安组织了南极天文

973 项目年度会议。

建立和完善了南极天文数据库，收集了南极天文

选址和天文观测的 3TB（压缩后）的数据。

南极天文科考支撑平台的修复与改进工作进行

中，测试了新的铱星通讯系统 PILOT II。

通过 CSTAR 望远镜改造的“南极高精度测光望

远镜”也已完成并在漠河测试。


6

在科学研究方面，依托 2012 年度申请成功的 973

项目“面向南极冰穹 A 中国南极天文台建设的天文观

测关键技术和天体物理重大问题”（973 项目首席为

王力帆研究员），原已基本成形的南极天文中心的各

个科学相关领域团组更加明确，形成了以宇宙大尺度

结构、星系和活动星系核、超新星与伽马暴、恒星、

系外行星等 5 个科研领域为主的科研团组。面向天文

学“两暗一黑三起源”重大科学问题，巩固和提升了

南极天文在国际天文学界的影响力。在首台南极巡天

望远镜 AST3-1 的工作期间，南极天文中心的各小组

成员完成了在“系外行星探测（CSTAR）”、“变星

的研究（CSTAR）”、“光变曲线特征的研究”、“伽

马暴光学对应体的研究”、“超新星的极早期探测的

研究”、“引力透镜效应的研究”等领域的预研工作，

使得南极天文中心在得到南极天文观测数据后能够

及时的发表有国际影响力的科研成果。

南极天文中心 2013 年度的科研工作阶段进展及

成果如下：

1）在仪器建设方面：完成了 AST－2 的研制工

作，并且已经在漠河测试基地测试运行。在发现问题

后进行了 CCD 导热和望远镜指向、跟踪的改进工作。

南极测光望远镜成功改造并且在漠河基地测试运行。

CCD 有本底较高和制冷的问题，已经运往英国修复。

南极天文科考支撑平台的修复改造正在进行中，更换

了铱星通讯系统。购买了南极天文中心新的数据服务

器。并设计了新的数据存储系统，可以便捷安全的储

存海量的 AST3 天文观测数据。为了更好的规范南极

天文设备的研制、运行、管理以及南极科考的准备与

管理、天文观测数据及成果的管理等，南极天文中心

成功的制定并向国家提交了“南极天文观测指南”。

2）在科学研究方面：使用 AST3 数据在不同的

科学领域进行深层次的科学研究，正在有条不紊的进

行，顺利通过了 973 项目“面向南极冰穹 A 中国南极

天文台建设的天文观测关键技术和天体物理重大问

题”，确立了以宇宙大尺度结构、星系和活动星系核、

超新星与伽马暴、恒星、系外行星为主的研究领域。

在宇宙大尺度机构的研究领域中，已经明确了如

下四个研究方向：基本宇宙学参数测量、暗物质性质

研究、星系形成的统计研究、暗能量的宇宙学检验。

并完善了相关的数据处理软件。结合国内在数值模拟

和理论模型上的研究优势，为探讨暗物质和暗能量、

第一代恒星和星系的形成、星系的形成和演化的一系

列关键科学问题提供保障

在星系和活动星系和的研究领域中，已经明确了

如下 5 个研究方向：星系与活动星系核的共同演化、

活动星系核光变与能源机制、黑洞潮汐撕碎恒星事件、

活动星系核的成团性分析、活动星系核核区几何结构。

基于南极冰穹 A 的极佳观测环境，以及每年长达四个

半月的极夜事件，AST3 的光变曲线质量将远优于其

他地面观测设备得到光变曲线。基于 SDSS stripe82

数据，对光变曲线特征研究的各种软件程序已经基本

成熟。

在宇宙伽玛暴领域研究取得如下成果：

1）对去年发现的超长伽玛暴 GRB 121027A，我

们（Wu, Hou & Lei, 2013, ApJL, 767, L36）在理论上

用大质量恒星死亡时物质抛射然后回落到中心黑洞，

并通过黑洞-吸积盘磁过程（Blandford-Znajek 机制）

产生长时间 X 射线辐射，成功解释了该暴中观测到的

长达几万秒的明亮 X 射线辐射。此工作被今年国际上

其他组关于超长伽玛暴观测和理论模型的 3 篇 SCI 论

文独立引用。

2）详细研究了双中子星并合引力波事件的电

磁辐射，如果并合产物是大质量强磁场中子星而非传

统认为的黑洞，那么这类引力波暴的电磁辐射（X 射

线、光学、射电）将非常强，我们在理论上首次详细

得研究了该类电磁辐射的光变曲线（Gao, Ding, Wu,

Zhang, & Dai, 2013, ApJ, 771, 86）。该工作被国际同

行在 2013 年发表的 SCI 论文中他引 6 篇次，另外还

有 4 篇国际同行的工作（2013 年尚未正式发表）也引

用了我们的工作，其中包括 Edo Berger 即将在 2014

年 Annual Reviews of Astronomy and Astrophysics 发

表的综述中引用。这对未来南极巡天望远镜对这类暂

现源的巡天具有重要的指导意义。同时我们也研究了

这类事件的高能中微子辐射和宇宙线产生（ Gao,

Zhang, Wu, & Dai, 2013, PRD, 88, d3010）。

2013 年度已发表的一般性工作（10 篇 SCI 论文

+1 篇国际会议论文）：

利用更大样本的伽玛暴 Liang-Zhang 关系，对宇

宙学模型（标准 Lambda CDM 模型和 Rh=ct 宇宙学）

及其参数进行了限制（Wei, Wu, & Melia, 2013, ApJ，

772，43）。

在统计上发现了伽玛暴中，时标越长的暴，其各


7

向同性辐射能量也越大的趋势，并用吸积模型尝试解

释，研究成果在 2012 年国际天文学年会分会中张贴，

并在 2013 年发表在此次会议的会议文集中（Hou, Liu,

Lin, Wu, & Lu, 2013, IAUS, 290, 223）。

在理论上较好地解释了今年发现的极端高能爆

发伽玛暴 GRB 130427A（Liu, Wang & Wu, 2013,

ApJL, 773, L20）。该工作获得了国际同行的 3 次他引，

其中包括 Fermi 卫星组和意大利研究组发表在

Science 杂志上的 2 篇工作对我们工作的引用。

对伽玛暴光学余辉样本进行了分析和统计，特别

是光学早期余辉的峰值辐射和后期的增亮现象，结合

理论模型对伽玛暴暴周环境、激波电子能谱指数分布

等参数进行了计算和统计，详见 Liang, Li, Gao, Zhang,

Liang, Wu, et al., 2013, ApJ, 774, 13。该工作发表以来，

在 2013 年获得国际同行他引 5 篇次。

对 2013 年发现的重要的短暴 GRB 130603B 的多

波段余辉，特别是后期增亮现象，给出了理论解释（Jin,

Xu, Fan, Wu & Wei, 2013, ApJL, 775, L19； Fan, Yu,

Xu, Jin, Wu, Wei & Zhang, 2013, ApJL, 779, L25）。其

中，Jin 一文被国际同行他引 3 篇次。

在理论上详细研究了伽玛暴不同环境下早期光

学余辉的时间行为（Yi, Wu & Dai 2013, ApJ, 776,

120），通过分析解方式给出了早期正反激波过程的

详细动力学演化和辐射演化。

对存在后期能量注入情形下的晚期余辉在理论

上进行了详细研究，对存在后期余辉突然增亮的 2 个

伽玛暴 GRB 081029 和 GRB 100621A 给出了很好的模

型拟合和解释（Geng, Wu, Huang, & Yu, 2013, ApJ,

779, 28）。

重新检查了短伽玛暴平台相辐射的观测数据，结

合双中子星并合模型，提出双中子星并合产物是大质

量毫秒转动的磁星，而且在短伽玛暴平台相辐射期间，

磁星的自传能损主要是引力波辐射主导，而非国际上

通常认为的磁偶极辐射主导，详见 Fan, Wu & Wei,

2013, PRD, 88, f7304。

详细考虑了存在同步自吸收加热情况下的同步

辐射和同步自康普顿辐射，讨论了电子能谱在同步自

吸收加热下的改变，给出了一般情形下同步辐射和同

步自康普顿辐射的辐射能谱的分析表达式，详见 Gao,

Lei, Wu & Zhang, 2013, MNRAS, 435, 2520。

详细计算和整理了伽玛暴余辉外激波模型下所

有情形的分析解，此工作作为综述文章应邀发表在

New Astronomy Reviews 杂志上，详见 Gao, Lei, Zou,

Wu & Zhang, 2013, NewAR, 57, 141。

同时，为了更好的参加中国南极科学考察，并顺

利完成其中的南极天文科考内容，南极天文中心筹划

了中心内部成员的体能、野外训练内容，购买了必要

的装备，今后可以在中心内部提前选拔合格的科考队

员参加中国南极科学考察队。

星系宇宙学和暗能量研究

围绕紫台“一三五”培育方向，在星系形成、宇

宙大尺度结构、引力透镜和 X 射线星系团等方面开展

了研究。组织队伍成功申请到国家自然科学基金重点

项目，该项目以弱引力透镜巡天为主要研究对象，并

将特别针对南极 KDUST 望远镜开展预研工作。与此

同时，团组还积极承担了南极 AST3 望远镜的 973 课

题，并加入科学院先导 B 的研究队伍。

基于中德马普伙伴小组，团组继续与德国马普天

文所和国内主要天文研究单位开展合作和联合培养

研究生。

1）发现了限制暗物质性质的新观测

过去的 10 年来宇宙学研究的最重要发现就是宇

宙的加速膨胀和和谐宇宙学模型的建立。在这个模型

中，宇宙中的主要能量是暗能量，主要物质是暗物质，

而我们可直接观测的物质只占很小一部分。但是，对

于暗能量的本质并不清楚，同时，也不清楚暗物质是

冷暗物质还是热暗物质。传统上一般利用高红移的赖

曼森林来测量物质分布在小尺度上的功率谱，从而限

制温暗物质的质量。然而，由于高红移的观测样本太

小，测量存在较大误差，因此，如果能利用近邻的大

样本星系来限制暗物质质量将是非常有用的。

基于中德马普伙伴小组，通过与德国马普天文所

合作，我们利用中科院超算中心的计算机模拟了三种

不同质量的温暗物质模型下星系的形成过程，研究发

现：可以同时利用 SDSS 的恒星质量函数和

Tully-Fisher 关系来限制温暗物质的质量。我们发现，

对于温暗物质质量小于 1Kev 的模型，其不能同时拟

和这两个观测量。我们同时还发现，对于温暗物质模

型，其预言的暗晕质量－恒星质量关系要比冷暗物质


8

模型预言的要高。然而，由于目前 SDSS 观测的限制，

我们还不能通过直接测量这一关系来限制温暗物质

质量。我们的研究倾向于进一步支持冷暗物质模型。

我们的研究结果对于基于南极 AST3 观测的 973

项目和下一代计划（KDUST）有非常重要的影响，就

是我们可以利用 AST3 和 KDUST 望远镜给出的高分

别星系图像，测量星系－星系透镜现象，从而可以限

制星系的暗物质晕质量，进一步可以限制温暗物质质

量。

2）研究星系在小尺度上的成团性问题

星系形成的半解析模型被广泛用来研究星系涉

及的一系列物理过程：气体冷却、恒星形成、超新星

和黑洞的能量反馈、星族合成模型、尘埃消光等。目

前国际上有几个流行的半解析模型，包括德国马普，

英国 Durham，紫金山天文台的 Kang 等模型。

这些星系形成模型能很好的解释观测到的星系

统计性质，如恒星质量函数，冷气体含量，星系大尺

度成团性等。最近几年随着 SDSS 的发展，小质量星

系的两点相关函数在小尺度上测量得更加准确。研究

发现目前所有的模型预言的暗星系在小尺度上的成

团性都比观测的要高。这个问题引发了一系列解决方

案，如引入扰动幅度更小的宇宙学模型，温暗物质模

型等。然而，大部分研究并未真正指出模型在小尺度

相关性比观测高的主要原因是什么，而且也没回答这

个问题：在现有的模型下，是否可能拟和小尺度的相

关性？

我们首先利用慕尼黑的公开星表，比较了其模型

的两个主要版本。选取慕尼黑星表的一个重要原因是：

模型一(De Lucia et al.)预言的星系质量函数比观测高，

而小尺度的两点相关函数跟观测较为接近。模型二

(Guo et al.)相比模型一有很多改进，特别是能很好的

拟和星系的质量函数，但小尺度成团性比观测强。因

此，仔细比较这两个模型之家的差别能为我们提供星

系小尺度成团性问题的更多线索。我们发现，Guo 等

的模型预言的卫星星系比例在大质量暗晕内偏高，可

能的原因有两个。1）Guo 等的模型考虑了卫星星系

的气体冷却，因此可能质量增加过快。2）Guo 等模

型中卫星星系的瓦解效率偏低。同时，我们还发现这

两个模型在中等尺度上的成团性也比观测高。这主要

是这两个模型预言的卫星星系数目都比观测要高

30％。

我们同时还改进了紫金山天文台的 Kang 等半解

析模型，发现如果在卫星星系中引入较强的超信息能

量反馈，模型预言的星系两点相关函数则跟观测符合

得很好。

3）利用数值模拟研究星系并合过程中的剥离过

程

近年来，关于银河系的形成研究非常热门。理解

银河系的形成过程，特别是卫星星系的吸积，恒星流

等，不仅对研究星系形成有重要意义，更为理解我们

人类家园的形成提供了有价值的结果。然而，目前研

究并不是特别清除星系并合过程中的物质受潮汐力

影响的剥离过程，特别是恒星的剥离效率与星系的形

态之间的关系。

我们利用数值模拟研究了银河系大小的星系在

并合过程中的恒星物质剥离过程。研究发现，恒星的

剥离效率跟星系的形态有很大关系，对于盘状的卫星

星系，其星系盘上的恒星在并合后 10 亿之内基本上

被剥离，消失在主星系的暗晕内。而对于中心有核球

的卫星星系，由于其物质密度相对较高，其剥离效率

明显偏低，其物质剥离时标可长达宇宙学年龄，即超

过 140 亿年。我们的研究结果意味着银河系内的大部

分年龄偏老的卫星星系都没有盘结构，最多保留一个

中心核球。

我们的研究对于正开展的 AST3 南极巡天有重要

意义，特别是对于银河系内的恒星流研究有重要启发

作用。

星系中的恒星形成研究

2013 年各项研究工作进展顺利，对高红移星系水

线以及 CO 的研究，近邻亮红外星系和并和星系，以

及蓝致密矮星系等等的研究方面都取得了进展，成果

都已发表，详述如下：

1）高红移星系：

Alian Omont 和 Yang, Chen tao, Gao, Yu 等人利

用 IRAM Plateau de Bure interferometer (PdBI)，对六

个 Herschel Astrophysical Terahertz Large Area Survey

(H-ATLAS) 新发现的高红移被透镜的超亮星暴星系

内的水蒸汽的进行了探测。确定了高红移超亮红外星

暴星系中 H2O 谱线强度与高阶 CO 谱线强度相当，谱

线轮廓和线宽相似。以 PdBI 目前的灵敏度，水线在


9

Herschel 巡天发现的高红移透镜星系中能很容易的

被探测到。对光度扩大修正后，利用已有的透镜模型，

发现 LH2O 很强的依赖于红外光度，表明 H2O 线的红

外激发辐射的重要性。暗示出水蒸汽在 LIR ≳ 1013 L

⊙高红移星系倾向于有非常强的发射，而在近邻宇宙

中中没有如此强的的发射。此结果发表在 2013，A&A，

551，115

Chentao Yang 等人（2013，ApJ, 771, 24）利用

Herschel SPIRE 的 FTS 第一次系统地研究了红外星系

的亚毫米波段的水蒸气的转动发射线。在已经发表的

176 个 FTS 数据的星系中，其中 45 个至少探测到了

一个 H2O 的发射线。另外，H2O+和 H2

18O 也被探测

到。H2O 在大多数星系 FTS 谱线中是除了 CO 最强的

发射。5 条最重要的 H2O 线光度与 LIR 近线性相关。

我们发现 t LH2O/LIR 随着 f25/f60,的增加而下降，但与

f60/f100 没有相关性，可能说明比较温暖的尘埃对亚毫

米的 H2O 线的激发影响很小。整个样本的平均能谱分

布图与单个星系的能谱分布图和红外抽运加上碰撞

激发模型相符合。

Tan, Qinghua 等人（2013, ApJ, 776, 24）利用

IRAM PdBI 干涉阵对红移 z = 3.216 和 4.058 的两个

大质量非引力透镜的 Lyman break 星系的 CO 发射

进行深度搜寻。发现其中一个源有低的 CO 信噪比

（3.5sigma)，另一个源只获得探测灵敏度上限。根据

观测结果发现 CO 线比根据近邻 z=0-2.5 星系的 IR 和

CO 光度相关性得到的 CO 发射线强度要低 3-4 倍，说

明在这些星系中低的金属丰度使得 CO-H2 的转化因

子增加，即，对于给定的分子(H2)，CO 发射更弱。在

红移 z >3 中实际观测到的金属丰度比已经被证明的

这个红移段的模型预言的要低。如果我们的星系是普

遍的，则在红移 z >3 的星系中探测到的这些分子气

体可以挑战 ALMA 的观测。

2）近邻亮红外星系：

Meijerink, R. 和高煜等人对近邻亮红外星系

NGC6240 进行了 Herschel SPIRE FTS 谱线探测，总

共探测到 20 条谱线，包括 CO J = 4-3 到 J = 13 -12，

6 条 H2O 的转动线，和 [CI] 和 [N II] 精细结构线。

把 C 和 J 激波模型应用到 H2 谱线和 CO 转动谱，发

现 H2 谱线需要比 CO 谱线模型能量更强的激波激发。

从而得出结论当星际介质只有一小部分暴露在高速

激波中的时候大部分气体正被慢（10 km/ s）激波激

发，因此气体很快的损失掉它的高速的湍流运动能量。

而高的 CO/连续谱比率是激波存在的一个重要的判据。

此结果发表在 2013， ApJ， 762， 16

Wang, Junzhi 等人 (2013, RAA, 13, 270) 对近邻

的并和星系 NGC6240 给出了 Very Large Array (VLA)

A 阵的高分辨率(~ 1″)的 H2CO 脉泽和 5 GHz 射电连

续谱观测结果。得到两个 H2CO 发射聚区，其中一个

与重叠区域 CO 最强的发射峰相连，而另一个在南边

星系西南两个角分的地方。这两个 H2CO 发射聚区都

与红外 H2 发射相连，而 H2 发射被认为来自于激波

过后的分子气体。根据 H2CO 发射的分布，H2CO mega

脉泽有可能受到星暴而不是活动星系核的影响。射电

连续谱不能激发 H2CO mega 脉泽例子反转，因为在

NGC 6240 中的两个 H2CO 发射区没有与射电连续

发射相连。激波动力学通过与近红外 H2 发射相连可

以产生 mega 脉泽需要的 H2CO 粒子布居的反转。

3）蓝致密矮星系

Zhao, Yinghe 和 Gao, Yu 等人研究了一个相当大

样本（53 个星系）的蓝致密矮星系（BCDs）的气体

的和化学性质。给出了 E- 和 I- 型 BCD 星系的氧丰

度，恒星质量，气体质量，重子质量和气体成份之间

的相关性。其中 E- 和 I- 型 BCD 星系根据 Loose &

Thuan 的分类，展示出椭球的和不规则的外晕。I-type

BCDs 相关性的斜率与 E-type BCDs 内的相似。普遍

来说，重子质量的一定，E-type BCDs 比 I-type 有更

多地贫气体和富金属的星系。由此认为至少一部分

E-type BCDs 和 I-type BCDs 可能处在不同的演化阶段

和/或者有不同的前身。另外氧丰度和气体相关性的探

测显示出 BCDs 并不是在孤立的环境中形成的，而是

已经经历了气体的喷流和/或者并和。此结果发表在

2013，ApJ, 764, 44

分子云与恒星形成研究

2013 年度本团组在银河系分子云分布和性质、年

轻星吸积和外流活动、原双星多波段研究、原行星盘

结构和演化、系外行星大气等研究方向进行了研究。

国家基金委重点项目“银河画卷计划—CO 分子巡天”

项目实施顺利；继续完善南极 Dome A THz 望远镜关

于分子云与恒星形成以及原行星盘的科学目标研究；

参加国家基金委重大科研仪器设备研制专项“太赫兹

超导阵列成像系统”项目；参加“中等口径大视场光

学望远镜”项目的前期准备；指导在读博士和硕士研


10

究生共 15 名，毕业博士研究生 1 名；毕业硕士研究

生 1 名。在第三届“中智天文研讨会”等双边和国际

大会上进行了广泛深入的交流；通过多渠道的人员交

流加强了国际合作。

1）年轻星吸积活动的系统性研究

对年轻星的吸积活动进行了迄今最为系统的研

究，取得了系列成果。对猎户座 L1641 恒星形成区中

的 1390 颗年轻星，使用 Spitzer、WISE、 2MASS 和

XMM 档案数据以及项目组取得的光学光谱数据，得

出了年轻星的光谱型、消光量、年龄和吸积率，这是

迄今对年轻星吸积活动最为系统的研究，得出了吸积

率与中心星质量的关系、吸积率与中心星演化阶段的

关系，以及吸积活动的时变特性。发现原行星盘环绕

年轻星的频率约为 50%，这一频率不随中心星质量而

改变；吸积时变不能够解释质量相近中心星其吸积率

会有两个量级的差异的现象。研究还证实了该区域中

的 46 个过渡盘以及成团和孤立两种恒星形成模式并

存。研究发现过渡盘中心星比光学厚盘中心星年老，

但比无盘星年轻。通过对年轻星年龄分布的分析，发

现猎户座 L1641 区域的恒星形成活动在 2–3 百万年前

开始趋于活跃。研究结果发表在 ApJS。

2）国际上最大样本原双星巡天

使用 SMA 在 1.3 毫米和 850 微米波段的连续谱

观测数据，对位于近邻恒星形成区内的 33 个 0 类原

恒星进行了高空间分辨率研究，这一研究是国际上迄

今最大样本的原双星巡天。在这 33 个 0 类原恒星中，

发现它们是单星、双星、三重星和四重星的数目分别

是 12、14、5 和 2，得出的 0 类原恒星的多重星频率

和伴星比分别是 0.64 ± 0.08 和 0.91 ± 0.05,它们是 I

类年轻星相应数值的 2 倍以上，是主序恒星相应数值

的 3 到 4 倍，并且发现在 0 类原恒星中，多重星系统

与双星系统的比例是 0.50 ± 0.09，高于 I 类年轻星的

相应数值（0.31 ±0.07）和主序恒星的相应数值（小

于 0.2）。这些观测结果表明，随着原恒星演化，其

双重/多重性也发生变化。基于这些结果我们提出了关

于双星形成的序贯碎裂图像。研究结果发表在 ApJ。

3）原行星盘研究

使用辐射转移程序 MC3D,结合 LZK 21 等三颗年

轻星天体从光学到毫米波段的 SED 数据, 对 LZK 21

等三颗年轻星天体的原行星盘的结构进行了十分详

尽的模拟工作，结果表明在这三个天体中发生了尘埃

往盘的中面沉降的过程。我们发现尘埃和气体均匀混

合的盘模型高估了这三颗年轻星在 70 微米波段的观

测流量。为此我们引入了另一种模型，在模型中考虑

尘埃往盘的中面沉降的效果。拟合结果表明新模型能

够很好地解释这三个源的所有观测。因此，我们证认

出的这三个源是高分辨率观测研究尘埃向原行星盘

中面沉降过程的理想目标。研究结果发表在 RAA。

4）“银河画卷计划”进展顺利

截至 2013 年底共获得 580 平方度天区的 CO 及

其同位素 J=1-0 三条谱线观测资料。详细分析了银河

系红外尘泡 N4 的气体分布和气体运动学，发现红外

尘泡 N4 很可能是一个膨胀的环状结构，而不是球状

结构。计算得出其质量、尺度、柱密度和光学厚度等

物理量，利用 (J, J - H)颜色-星等图证认了该区域的大

质量恒星候选天体，发现其中一颗质量约为 15 M⊙，

年龄约为 1 百万年的大质量恒星候选天体很可能是红

外尘泡 N4 的激发源。在该区域还发现了气体下落的

证据。研究结果发表在 RAA。对其它 17 个红外尘泡

的性质也进行了深入分析，并在国际会议上报告了研

究结果。初步完成了 Aquila Rift、Rossete 等区域的论

文撰写。

5）系外行星大气研究

完成了对系外行星 HAT-P-1b 大气透射光谱资

料的处理和分析；申请并获得了 Palomar 5 米望远镜

对系外行星大气的观测时间 2 次，并成功完成了其中

一次的观测，获得了系外行星 HAT-P-32b 的大气透射

谱。另一次观测将在 2014 年 4 月执行。

6）银河系中心和河外星系分子气体研究

通过对银河系中心分子气体的多条 H2CO 谱线观

测研究，发现分子气体的温度普遍偏高，从 50 K 到

100 K，甚至更高。发现在大尺度上，高温气体可能

是由宇宙线加热或者湍动加热，而不大可能是由光子

加热或者 X-ray 加热。这一结果对研究遥远的极亮红

外星系中的剧烈星暴提供了重要参考。研究结果已经

在 A&A 杂志发表。利用 IRAM 30m 望远镜，对近邻

星系 NGC253 和超亮红外星系 Mrk 231 进行了 CN、

13CN 以及 CO 谱线观测，发现 NGC 253 星系中

12C/13C 的丰度比为 40，这个比值大于银河系 CMZ

区域的对应值，表明在 NGC 253 中有更多的气体进入

星系中心。研究结果已被 A&A 杂志接收。


11

毫米波与亚毫米波技术实验室

主要包括：1）南极 5 米太赫兹望远镜（DATE5）

预先研究，包括南极 5 米太赫兹望远镜系统及分系统

的方案设计，高精度太赫兹天线、高灵敏度超导混频

器、宽带数字频谱处理后端、低功耗 4K 低温制冷等

关键技术研究；2）国家重大科研仪器设备研制专项

“太赫兹超导阵列成像系统”和“多波段多大气成分

主被动综合探测系统-太赫兹辐射波谱仪”，研制进展

顺利，并通过基金委的年度检查和中科院的年度监理；

3）“太赫兹超导探测器研制平台一期”，转入常规运

行阶段，成功制备出第一批全制程超导隧道结芯片；

4）太赫兹频段超导相干和非相干探测技术研究及应

用，包括多波束接收机技术研究、太赫兹超导混频器

温度及频率相关性研究、超宽带太赫兹超导探测器研

制以及太赫兹测量平台构建等。

“太赫兹超导探测器研制平台一期”成功转入常

规运行阶段。制备出第一批全制程超导隧道结芯片等

器件，为实验室太赫兹超导探测器技术研究提供有力

支撑。“太赫兹超导探测器研制平台一期”共包含三

台主设备，分别为超导及金属薄膜磁控溅射系统、绝

缘层磁控溅射系统和掩膜对准光刻系统。自 2012 年 5

月通过验收后，经过近一年的状态调试，已成功转入

常规运行阶段。运行迄今，实验室已经可以自主溅镀

包括 Nb、Al、Ti 和 SiO2 在内的单层或多层金属及绝

缘层薄膜，重点制备的 Nb 膜溅射速率可以通过改变

直流电流或者射频功率进行良好控制。2013 年度，实

验室利用研制平台，成功制备出第一批全制程超导隧

道结芯片，质量因子高达 12 以上，该项工作是象征

研制平台溅射成功的标志性成果。利用该系列设备，

实验室还自主制备了国家重大科研仪器设备研制专

项“太赫兹超导阵列成像系统”项目中 TES 超导探测

器的 Ti 超导薄膜，制备了基于 Al 膜的周期结构等器

件。

国家重大科研仪器设备研制专项“太赫兹超导阵

列成像系统”关键技术取得突破，顺利通过基金委的

年度检查和中科院的年度监理。该项目在 2013 年度

进展顺利，完成了针对两种探测器阵列的低温光学系

统设计，以及 POST 望远镜与 0.3K 杜瓦间集成方案

设计；研制了基于 Nb 和 TiN 两种超导薄膜的 8×8 像

元超导动态电感探测器（MKIDs）阵列，实现 MKIDs

探测器阵列芯片的制备与亚 K 温区低温特性初步表

征，以及 MKIDs 频域读出复用单元的初步研制和测

试；实现单像元超导 TES 探测器特性表征，灵敏度达

到预期目标，并完成了 8×8 像元超导 TES 探测器阵

列芯片和时域读出复用单元方案的初步设计等。

南极 5 米太赫兹望远镜关键技术研究：完成南极

5 米太赫兹望远镜（DATE5）系统和分系统的方案设

计；完成了 H350 波段超导隧道结混频器的设计以及

芯片制备掩膜板的加工；完成了 H200 波段超导 HEB

混频器单元原理芯片的研制，性能处于国际前沿水平；

完成了 2GHz 带宽 FFTS 宽带高分辨率数字频谱仪的

研制；开展了高精度天线原型面板试制和全息测量技

术方案研究。另外，开始太赫兹本振源和 4K 低温制

冷等关键单元的初步试制。

太赫兹频段超导相干和非相干探测技术研究及

应用：开展了 NbN 太赫兹超导 SIS 隧道结直流与探

测器特性的温度相关性研究，太赫兹超导 HEB 混频

器频率与温度相关性研究，均取得原创性结果；实现

超宽带太赫兹超导探测器研制，成功应用于太赫兹测

量平台构建及波束特性近场测量等；基于太赫兹 TDS

和 VNA 测量技术，实现硅基材料介质特性的宽带测

量；开展了多波束超导 SIS 接收机关键技术研究。

青海观测站

13.7 米望远镜全年开机运行 294 天，其中对外开

放课题观测 294 天。2013 年度新受理课题观测申请

12 件，安排国内外申请的课题观测 20 件，完成 CO、

HCO+、CH3OH 等分子谱线的课题观测。2013 年度

望远镜平均每天扫描 1.5 平方度的天区。2013 年度无

论在设备运转、开放课题观测时间，还是在设备稳定

运行、数据产出量方面，继续保持历史高位，数据质

量则有更大提高。2013-2014 观测季节的开放课题观

测从 2013 年 9 月 20 日开始。

为降低副反射面热形变导致的测量误差，由中国

电子科技集团公司第五十四研究所研制，望远镜副反

射面成功更换为碳纤维材料。增加本振功率电调衰减

器装置，实现了远程调整本振输出功率的功能，大大

提高了工作效率；更换了超导成像频谱仪系统的部分

像元的 HEMT 放大器、在杜瓦内部 50K 冷级金属罩

贴防热辐射薄膜，改善接收机的稳定性，确保 “银

河画卷计划”工作顺利进行；截止到 2013 年年底，“银

河画卷计划”巡天工作 580 平方度的天区观测，包括


12

M17, Aqualia Rift, Cygnus X, W3/W4/W5, GEM OB1,

Monoceros Nebula, Maddalena Cloud, 和 Califirnia

Cloud 等比较有名的天体目标，对其中的分子云演化

和恒星形成过程进行了研究，数据质量完全符合科学

家的要求，彰显了“超导成像频谱仪系统+OTF 观测

模式”的强大威力。

银河系本地臂以往被认为只是一个刺，或者说一

个鼓包，青海观测站首席科学家徐烨研究员最新研究

结果发现，本地臂的形态和运动学与主臂类似，有

1kpc 宽，5kpc 长，本地臂的整体运动比银河系的转

动慢 5km/s。这是天文学历史上首次精确测定旋臂结

构的三维运动。该工作表明精确测量银河系旋臂已经

成为现实。这一结果对银河系经典旋臂理论是一个巨

大挑战，因为传统的密度波理论认为银河系只能有 4

条或者 2 条主臂，而本地臂是不能存在的。这个工作

在 2013 年 6 月举行的美国天文学会第 222 次会议上，

作为亮点工作被介绍，并受到《U.S．News and World’

s Report （美国新闻与世界报道）》、《 SPACE 》、

《Universe Today》和 NRAO(美国国家射电天文台)

等知名媒体的采访报道，国内的中央电视台、新华社、

人民日报等媒体也介绍了这项科研成果。

青海观测站科研人员经常在一些国际大会上作

大会主题报告（或者特邀综述报告）并担任科学委员

会成员。基地的科研人员在国际上有很高的显示度，

资深天文学家 Caswell 撰写的关于银河系结构的综述

文章中，认为徐烨等人的系列工作是银河系结构领域

里的一个里程碑。

甲醇脉泽是研究大质量恒星形成的重要探针，是

探索恒星形成区激波等物理环境及天体距离测量的

有效工具。上海天文台陈曦博士主导的研究团队，用

13.7 米射电望远镜首次开展大型 I 型甲醇脉泽的巡天

工作，目前已探测到了 200 多颗新的 I 型甲醇脉泽源，

其数目是过去国际上几十年来 I 型甲醇脉泽探测数目

的总和，为进一步完备银河系内甲醇脉泽源星表奠定

了基础，并有多篇文章发表在 ApJ 或 ApJS 杂志上。

该工作得到了国内外同行专家的认可，并特邀为《科

学通报》杂志撰写综述文章（英文版）。

北京大学吴月芳课题组，利用基地望远镜研究结

果表明：CO 的丰度可以示踪分子云的演化；对云云

碰撞是大质量恒星触发机制进行了进一步的观测验

证；对金牛座－英仙座－加利福尼亚云中普朗克冷尘

块进行了分子谱线成图观测，运用辐射传能理论计算

出了激发温度、柱密度，质量和热致宽、非热致宽以

及 3 维线宽等物理参数。

2013 年 11 月底，开始安装 SONG 项 1 米光学望

远镜，12 月初开始安装后端光谱仪系统，正在进一步

调试阶段。50Bin 望远镜正在进行实验性观测。

作为青海省爱国主义和科普教育基地，继续承担

着爱国主义教育和科普宣传的任务，配合当地政府开

展一系列天文科普宣传工作。由海西州政府与紫金山

天文台共建的“德令哈天文科普馆”项目土建工程全

部结束，正在进行内部陈展装修、外部广场建设工作。

继续实施园区建设计划，对大门外、站区道路进

行了维护；在专项资金的支持下，对值班休息室进行

了扩容，绿化观测站区等。为望远镜运行和来访观测

人员提供了良好的工作和生活条件。

III. 应用天体力学和空间目标与碎片研究部

空间目标与碎片观测研究中心

2013 年度团组在科研、重大设备研制、完成国家

任务以及观测网的持续运行等各方面开展了大量工

作，主要有：1）院观测网持续运行，目标管理能力

持续增长；2）圆满完成多项国家任务，特别是“天

宫一号/神舟十号”空间碎片预警监测任务；3）院配

套基建项目顺利进行，完成了基建项目的财务审计工

作； 4）30 厘米参与了入网试验工作，全系统进入试

运行观测阶段；5）完成了 90 厘米望远镜和捆绑望远

镜外场检测工作；6）2013 年上半年完成了修购项目：

观测网升级改造项目的全部内容；2013 年 11 月完成

了修购项目：洪河多目标探测系统升级改造（一期）

的全部内容。7）继续开展轨道动力学、空间碎片观

测方面的相关科研工作，主要有：同步轨道、半同步

轨道、Molniya 和 Tundra 型轨道动力学特征及其长期

演化规律研究、编目技术﹑陨落期预报方法、天文定

位、识别方法、大气模型改进﹑碰撞预警、空间碎片

测光方法﹑暗弱目标探测方法以及空间碎片观测研

究；8）完成了“十一五”空间碎片 3 个项目的验收；

“十二五”空间碎片 3 个项目通过了国防科工局专家

组的中期检查。9）2013 年度，团组在研课题共计 38

项，并完成了其中 9 项课题的结题与验收工作，新申

请到课题 7 项。

2013 年中心参加了多项国家任务，并得到了各方


13

好评。主要有：①韩国卫星和火箭监测任务；②我国

“遥感 7 号”卫星与俄罗斯“旋风 3 号”火箭碰撞预

警任务；③俄罗斯卫星 BLITS 事件分析；④厄瓜多尔

“飞马座”卫星与俄罗斯“旋风三号”火箭近距离交

会事件分析；⑤“天宫一号/神舟十号”碰撞预警监测

任务；⑥我国“海洋一号 B”卫星与俄罗斯“宇宙 3M”

火箭碰撞预警监测任务；⑦我国火箭发射减缓辅助评

估；⑧欧空局 GOCE 卫星陨落期预报任务；⑨低轨道

火箭光度国际联测试验；⑩中高轨目标编目任务。特

别在“天宫一号/神舟十号”空间碎片预警监测任务中，

中心全网观测设备采集的观测数据，占整个观测数据

的一半以上，其中大椭圆轨道空间碎片的数据量占 90%

以上，保障了“天宫一号/神舟十号”的飞行安全，发

挥了不可替代的重要作用，为我院争得了荣誉；2013

年上、下半年各执行 1 次国家重要任务，2 次任务执

行时间累计超过 6 个月，均顺利完成相关工作。

90 厘米项目于 2013 年 9 月完成了专家组建议的

密封性好改正镜组的安装并已完成外场检测试。运行

阶段，90 厘米望远镜参加了多项重要国家任务，并成

功观测到小行星 1998QE2；捆绑式望远镜于 2013 年 5

月在姚安站完成安装调试，并在 2013 年 9 月完成了

望远镜的外场检测，等待专家组组织安排验收；院观

测系统配套基建项目已完成全部内容，基建部分已完

成财务审计；空间碎片专项“十一五”课题 3 项已完

成验收，“十二五”空间碎片课题 3 项已通过中期检

查。天文定位、识别方法应用于我国首颗天基探测卫

星中，在中心指向误差较大的情况下，实现了实时天

文定位。

课题研究方面进展情况：继续深入开展人造天体

的一些特殊轨道的长期演化规律、空间碎片的观测方

法、空间碎片非质点的旋转运动特征提取及分析等方

面的工作。

基于轨道共振的思想，研究了半同步轨道带物体

运动的二维相平面结构及其稳定性。研究表明：传统

的只考虑 J32 项的 12h 近圆轨道卫星的理想共振模型

不具有普适性，不适用于轨道倾角处于 67-74 度的半

同步轨道带物体，因为其深共振项是 J44 项。

深入分析了同步、半同步轨道带物体轨道面的演

化规律及轨道倾角的变化范围，并解释了其力学机制。

研究表明，这种进动主要是由地球扁率摄动引起的绕

地球自转轴进动，二阶太阳引力摄动引起的绕太阳黄

道面法向矢量进动和二阶月球引力摄动引起的绕月

球白道面法向矢量进动的合成。

从理论上探讨了 Molniya 型轨道在地球引力作用

下的长期演化特征。结果表明：对于大面质比物体，

轨道偏心率和轨道倾角呈现较大的变化幅度，

Molniya 型轨道的特征不再保持。轨道长期演化以及

轨道寿命显著依赖于初始升交点经度和面质比，且对

初值极其敏感。

研究了参考轨道为椭圆轨道的低轨“伴飞”轨道

的长期演化。考虑四阶地球非球形引力场对“伴飞”

轨道的摄动影响，得到了保持构型稳定的条件：参考

轨道和“伴飞”轨道的半长径的变化率一致。

深入研究了高轨空间碎片的观测方法。为了满足

空间碎片光学观测高精度与实时性的要求，提出了一

种 CCD 图像处理方法。基于高轨目标实测图像的实

验结果表明，该方法计算得到的赤经精度优于 0.2 象

素，赤纬精度优于 0.1 象素；处理图像的时间约为

0.2 秒，处理图像的时间约为 0.8 秒，满足高轨空间

碎片数据处理的要求。为了解决空间碎片观测中存在

诸多图像退化因素，提出了一种空间域的图像处理方

法，结果表明：该方法较好地处理了星像的退化，提

升了星像的信噪比与定位精度。

在对光度信息进行归一化处理的基础上，统计和

分析了大量低轨空间碎片的光度数据，给出了光度分

布结果，分析了小相位角和大相位角情况下空间碎片

视亮度的变化，发现空间碎片相位角和星等间呈现出

复杂的关系，偏离了理论的描述。通过模拟研究，验

证了空间碎片受重力梯度力矩影响下旋转状态的短

期和长期演化。

研究了高层大气模型主参数的短期改正方法。提

出了利用星载高精度大气实测资料对大气模型主参

数进行短期改正，从 110 个大气模型参数中甄别筛选

出具有代表意义、稳定、可解的主参数 13 个，得到

了适用于较短时间、局部空间内的大气模型（测试用），

并应用于某卫星的轨道预报中。结果表明，测试模型

能提高轨道预报精度 7%-60%（成功率接近 70%）。此

外，我们还研究了太阳辐射指数的中期预报方法，能

根据以往 5 个太阳自转周到历史指数预报未来 54 天

的辐射指数 F10.7，精度显著优于传统的三角函数预

报法。

开展空间碎片和监测目标轨道误差生成和演技

术的研究工作。调研了国内外的轨道确定及误差生


14

成技术；根据轨道特征，将自主编目目标进行分类，

利用定轨标校预报的方法对其轨道精度进行评估，并

通过统计的方法对轨道误差演化规律进行建模，给出

了不同类型目标的轨道误差演化拟合系数公式；从理

论上研究了目标的轨道协方差生成与演化技术，并利

用自主数据进行了轨道协方差的数值演化验证。

完成国家自然基金面上项目，建立了低轨道空间

目标跟踪调度优化模型、中高轨道空间目标跟踪调度

优化模型以及空间目标的分配模型；形成优化软件，

系统的建立了空间目标跟踪调度数学框架，同时具有

很强的实用性，当前计算能力能够满足计算需求，计

算时间能够满足日常使用的需要。

卫星精密定轨及应用研究

CCD 相机研制实验室

围绕紫台战略发展方向，结合大视场望远镜的需

求，积极开展大靶面 CCD 拼接相机的研究；结合我

台空间目标观测的需求，开展高速 CCD 相机的研制；

考虑到未来的发展需求，进行 CCD 新技术的研究和

储备。

完成高速大靶面拼接 CCD 相机的样机研制。成

像靶面 152mm×152mm，四芯片拼接，千兆网数据输

出，读出速度为 1.5FPS，制冷方式：TE+水冷，制冷

温度达到﹣30°C（室温@+20°C），读出噪声为 8 个电

子（@3M Pexil）,暗流≤0.03 电子（@-20°C）。

大口径高速卷帘式快门样机的研制成功。快门通

光口径＞400mm×400mm，快门开启速度小于 1 秒，

快门工作时无快门效应，快门在通光光轴方向上挡光

少。为我国研制大靶面的拼接 CCD 相机提供了技术

保障。

完成我国中等口径大视场望远镜的主焦面装置

的方案设计。拼接 CCD 相机，10k×10k×9 个芯片=9

亿像元，成像靶面直径≥360mm，压缩机深度制冷系

统，CCD 相机工作温度低于-100°C，磁定位的 6 波段

的滤光片系统，像场旋转器等。

光纤接口的 CCD 相机样机研制，已成功研制出

利用光纤接口的 CCD 相机，传输距离大于 2000m，

数据传输保密性好，为 CCD 相机的国防应用打下了

基础。

IV. 行星科学和深空探测研究部

近地天体探测和太阳系天体研究

开展了彗星观测和研究、海王星特洛伊 2011

HM102 的稳定性研究，以及木星和土星的逆行卫星起

源的研究，并参与小行星深空探测开展了系列调研、

研讨和相关研究工作，参加中国科学院行星科学重点

实验室成立和运行工作。研究远距离彗星的活动性及

其活动机制，分析研究了 2011 年 4 月获取的 4 颗彗

星的观测数据，完成的研究论文已投稿 MNRAS，正

在审理之中。深入调研了特洛伊小行星的形成和演化

的研究现状，对其轨道演化及形成稳定区域的机制进

行了初步分析研究，针对海王星特洛伊 2011 HM102

的稳定性研究，已作出初步结果。

远距离彗星的活动性和活动机制研究：对远距离

彗星 228P/LINEAR ， C/2006 S3 (LONEOS) 和

29P/Schwassmann-Wachmann 1 进行观测和测光研究，

得出了这些彗星的彗核半径上限、表面亮度轮廓、彗

发颜色以及 Afρ值和尘埃生成率等物理参数，并利用

一些图像处理方法研究彗发中可能存在的结构特征，

最后对这些彗星在大的日心距保持活动性的原因进

行了分析。结果显示（1）彗星 228P/LINEAR，C/2006

S3 (LONEOS) 和 29P/Schwassmann-Wachmann 1 在

日心距大于 3 AU 处都具有明显的活动性，2）彗星的

表面亮度轮廓梯度差异明显，对彗星

29P/Schwassmann-Wachmann 1 ，内部区域亮度轮廓

较陡，这可用彗核附近存在一个“加速度区”来解释，

在这个区域内，从彗核抛出的尘埃颗粒被加速到终极

速度，外部区域与其他彗星相同，是由于彗核源区的

活动性变化引起的。

海王星特洛伊 2011 HM102 的稳定性研究：海王

星特洛伊 2011 HM102 的稳定性研究，模型：太阳 +

四个气巨星 + the clone of HM102，只考虑相互之间

的引力作用，忽略克隆体的质量，结果：在时间区间

-0.5Gyr 到 2.7Gyr 内，所有克隆体均稳定；从各根数

的分布图可初步推测其相图结构。

历算和天文参考系研究

完成了常规天文历书编算工作，开展了《电子航

海天文历》研制和《航海天文历》编算规范制定等工

作，此外还就天文历书服务规范化和信息化工作向国


15

家多个部门提出了建议或提交了申请书。

在太阳系主要天体基本历表研究方面，完成了观

测资料归算和历表拟合模块的建立和验证工作，同时

还开展了自主观测及相关的研究工作。此外，在光传

播、引力理论、物质间第五种相互作用等方面发表了

多篇研究论文。

在双星和多星系统运动理论研究方面，发表了一

篇单谱线分光双星光心轨道拟合工作，并在双星系统

轨道视差和子星质量确定方面取得了较大进展。此外，

等级三星系统运动学模型及动力学稳定性等课题研

究也取得了一定进展。

参加院学部基本天文学及其应用发展战略研究

工作，提交了我国历书天文学发展战略规划初稿，其

中分别就历书天文学研究和天文历书服务两个方面

提出了相应的重点发展方向、目标和建议，由此也进

一步明确了本团组围绕我台重点培育方向“行星科学

与历书天文、深空探测”拟开展的科研工作内容，主

要包括天文历书服务规范化和信息化，以及太阳系主

要天体和双星、多星的子星运动理论及其相关研究。

本年度在完成常规天文历书编算工作的同时，通

过增加天然卫星视位置历表进一步丰富了天文历书

网络服务的内容，此外还在天文历书服务规范化和信

息化方面开展了以下几项工作：初步完成了《电子航

海天文历》的研制工作，开展了《航海天文历》编算

规范制定工作，就天文航海信息系统研制向海军司令

部提交了项目建议书，就制定农历编算标准和规范农

历颁行工作向国家有关部门提出了建议，就天文历书

服务规范研制提出了国家科技基础性工作专项重大

需求建议。这些阶段性工作进展为全面建立我国规范

的天文历书信息化服务系统打下了良好基础。

太阳系主要天体基本历表研究取得阶段性进展：

完成了各种主要观测资料归算模块的建立和验证工

作，同时开展了一些自主观测及相关的研究工作，获

得了有关天体的 127 张底片资料；完成了历表拟合模

块的建立和验证工作。这些阶段性工作进展与有关课

题合作单位关于太阳系小天体摄动模型的研究进展

一起为以后顺利完成自主太阳系主要天体基本历表

的研制工作提供了保证。与本研究方向相关的一项已

发表于 MNRAS 上的亮点工作是：提出了两种探测物

质之间是否存在第五种相互作用的可能方法，即卫星

钟和地面钟之间的比对，以及对卫星钟轨道近点进动

的长期观测。

双星和多星系统运动理论方面：1）得到了 72 颗

单谱线分光双星光心的可靠轨道（发表于 AJ）。通过

对此前拟合过程的重要改进，即不仅放弃了此前拟合

过程中的一个不恰当简化近似，而且发展了一种高效

的网格拟合方法，该方法不仅通过引进一个只含单个

非线性分量的拟合参数矢量降低了网格维数，而且通

过在局部线性化意义下使非线性参数也参与拟合的

办法大大减少了所需的网格点数。该方法同样适用于

利用已可预见的海量 Gaia 资料开展的类似工作，因

此对今后的双星轨道拟合工作具有重要意义。2）得

到了子星均为主序星且已知星等的 455 个双星系统的

轨道视差和子星质量。3）初步完成了等级三星系统

一阶分析运动学模型的建立工作，并且在此类系统动

力学稳定性研究方面也取得了一定进展。

太阳和太阳系等离子体研究

2013 年度主要在以下几个方面取得了一定进展：

太阳大气和太阳风中动力学阿尔文波的激发与

产生机制：动力学阿尔文波在太阳大气和太阳风非均

匀加热现象中可能起重要的关键作用。在本年度中，

我们进一步研究了太阳大气和太阳风中动力学阿尔

文波的激发与产生机制，结果显示等离子体的“场向

密度纹”和“场向电流”都能够通过等离子体不稳定

性直接、有效地激发动力学阿尔文波的产生，而大量

的观测表明这类“场向密度纹”和“场向电流”作为

“丝化纤维”和“载流环”普遍存在于太阳磁等离子

体大气中。同时，我们也研究了在太阳风和太阳大气

中通过非线性波波耦合和参数衰变过程产生动力学

阿尔文波的可能性；

太阳射电爆发活动中的阿尔文波和电子回旋脉

泽辐射：阿尔文波是普遍存在于太阳和空间等离子体

中的低频电磁扰动，电子回旋脉泽辐射是太阳射电物

理中最重要的高频电磁波辐射机制之一。我们近来针

对阿尔文波的激发和产生机制、阿尔文波对电子回旋

脉泽辐射机制的影响、以及它们在太阳射电爆发现象

中的应用等问题进行了一系列研究，结果显示背景等

离子体中的阿尔文波对回旋脉泽辐射将产生重要的

影响，不仅改变了回旋共振条件，而且也影响到电磁

辐射的偏振特性和辐射条件。特别是，对于太阳射电

爆发现象中长期未能很好理解的太阳射电暴问题，我


16

们基于这一理论提出一个比较合理的物理模型；

太阳大气中高能电子束的传播与能谱演化：高能

电子束在太阳大气传播过程中的能量损失和能谱演

化一直是太阳活动现象中吸引着广泛兴趣的一个研

究课题。具有较高能谱和空间分辩率的 RHESSI 卫星

观测为这项研究提供了一个很好的机会。我们最近基

于 RHESSI 的观测分析，发现电子束流－回流系统中

可能存在的反常电阻能合理地解释 RHESSI 观测到的

硬 X 射线环顶源和环足源之间的能谱演化，意味着反

常电阻在束流－回流系统的动力学演化中可能起重

要作用。

天体化学和行星科学实验室

能力建设方面：完成了财政部 2013 年修购计划”

天体化学实验平台一期”项目建设工作，引进了电子

探针、阴极发光探测器、拉曼光谱仪、能谱仪、背散

射电子衍射仪、精密切割机、蒸镀仪等实验设备，完

善了紫台天体化学实验室的测试功能；协助完成了中

国科学院行星科学重点实验室的建设工作；

研究进展方面：在 NWA 2339 eucrite 中发现了辉

石和长石的硫化交代反应现象, 研究表明灶神星表面

的挥发组分比预期高很多，在冲击变质过程中，硫进

入硅酸盐矿物中。研究成果发表在<Geochimica et

Cosmochimica Acta>；开展火星陨石的研究工作，在

NWA 2737 火星陨石中发现含水矿物角闪石，获得了

火星岩浆含水量的数据，研究成果发表在<Meteoritics

& Planetary Science>。

盱眙天文观测站

2013 年度近地天体望远镜 1-4 月使用 4kCCD，

6-10 月使用 10kCCD，除了 5 月份更换 CCD 和其他

几天设备维护外，总的开机天数为 355 天。盱眙站天

气情况，全晴夜天数是 160 天。考虑月光夜影响，以

及半夜是晴天的情况，根据所拍摄图像数量进行折算，

在 2013 年度有效观测夜 134 夜，拍摄图像 49737 幅。

开展太阳系天体巡天观测，共计获得 99655 个太

阳系小天体的 550622 个观测数据，在全球 464 个台

站中观测量据第五，在观测量最多的十个大站中精度

最高，使得我台乃至我国的太阳系小天体观测上了一

个新的台阶。

2013 年的工作主线是围绕近地天体观测系统的

软硬件升级和正常观测使用开展。

能力建设方面：1）继续修购项目“近地天体望

远镜终端升级改造”。完成了 10k 大靶面 CCD 相机的

升级安装和试观测。完成了近地天体望远镜光机改造

升级、数据存储服务器、大靶面滤光片组的定制。目

前近地天体望远镜视场为 3 度 X3 度，象元分辨率为

1.02 角秒X1.02 角秒，配置了 SDSS-griz，Bessel-BVRI、

和 VR，Ha，O3，S2 三组滤光片。开展了近地天体望

远镜控制软件系统（c3）的集成，完成了近地天体望

远镜伺服、STA 相机控制、Bonn 快门、盱眙站气象、

观测任务列表等信息的 web 访问终端，实现了观测的

自动化和网络化。极大的提高了观测的稳定性和效率。

2）开展了紫台重点数据库应用示范项目--近地天体望

远镜数据库系统的升级，采用 MongoDB 数据库系统，

实现了观测数据的实时入库、管理和发布。完成了盱

眙观测站夜天光监测系统项目，实现了盱眙站温度、

湿度、气压、风向、风速、夜天光、视宁度等信息的

采集、记录和管理。

运行方面：本年度继续开展太阳系小天体的观测

巡天，共计获得 99655 个太阳系小天体的 550622 个

观测数据，在全球 464 个台站中观测量据第五。在观

测量最多的十个大站中精度最高。

研究方面：继续小行星形状重建的观测，与美国

Butler 大学的韩先明教授等合作开展了小行星光变国

际联测，已发表论文 6 篇；与澳科大进行了小行星形

状重建研究，已发表论文 2 篇。通过合作研究，完成

了反银心方向巡天观测的补充观测；进行了北天窄波

段巡天观测的试观测、开展 40cm 双筒望远镜观测资

料文档的电子化和底片库改造等合作项目。

推进项目进展：根据紫台发展要求，参与了中等

口径大视场望远镜的科学目标的论证。全程参与了大

视场望远镜的光学和机械设计的讨论。开展了我国近

地天体监测预警中心的规划。2013 年 2 月为国务院应

急办提供了车里雅宾斯克陨石事件的咨询，4 月向科

学院提交了“关于成立国家近地天体监测预警研究中

心的建议书”，获得国务院相关部门的批复，完善了

建议书。

行星科学与深空探测实验室（筹）

2013 年 4 月经中科院批复，成立了《中国科学院


17

行星科学重点实验室》，依托于中科院上海天文台和

紫金山天文台。该重点实验室面向行星科学基础前沿、

我国自主行星深空探测计划创新性科学目标的制定，

其总体目标为：成为我国开展行星科学国际前沿基础

研究、承研国家有关深空探测重大科技专项任务以及

培养高水平研究人才的一个重要研究机构。

1）小行星深空探测方面：

（a）4179 号小行星图塔蒂斯研究取得重要进展：

利用嫦娥二号探测器对 4179 号小行星图塔蒂斯飞越

探测获取的光学图像，重点研究了该小行星的物理特

性、表面特征、内部结构以及可能的起源等（Huang,

Ji & Ye et al., 2013, Scientific Reports）。

研究结果表明，嫦娥二号距图塔蒂斯表面最近的

距离约为 770 米，获得最高分辨率光学图像优于 3 米

/像素。基于所获取的图像，结合探测器的轨道与姿态

信息，确定了图塔蒂斯主轴的空间指向。从图像估算

了小行星尺寸，长度和宽度不超过 4.75 × 1.95 （±

10%）千米。

通过对嫦娥二号高分辨率观测资料的分析，发现

了一些以往地面雷达观测中未曾发现的新特征：图塔

蒂斯形似一根生姜，由较小的一端“头部”与较大的

一端“身体”组成；在“身体”端部存在一个直径大

约 800 米的巨型盆地，在小行星的表面找到了超过 50

处较为明显的、大小不一的陨石坑，其中包括两个先

后产生在同一位置附近相互有部分遮盖的陨坑；“颈

部”则以近乎垂直角度连接着“头部”和“身体”；

其表面存在超过 30 个有巨石特征的区域；从其结构

特征可推断图塔蒂斯很可能是一颗具有碎石堆结构

的密近双小行星，可能由两个独立小天体缓慢靠近形

成，可能是约普(YORP)效应作用或是大规模的撞击造

成。

该成果入选 2012 年度“十大天文科技进展”，是

探月工程（二期）的重要成果，也是我国在此首次行

星际探测活动中，多目标新模式探测、小行星新领域

开拓的成功尝试，工程实践与科学研究相融合的成功

范例，获得国际同行关注与好评。Nature 网站首页头

条推介此成果，中文版推荐为研究亮点，全球多个知

名媒体也进行了全面报道。

（b）有机组分分析仪原理样机研制取得重要进

展：与协作单位积极沟通交流，共同推进有机组分分

析仪前端钻取采样密封加热一体化装置的原理样机

研制工作，目前已按照预期目标完成了钻杆旋转机构

驱动组件、钻头组件、体积测量组件和密封组件等研

制，并已完成了特种金刚石钻头干钻岩石试验，测试

试验结果表明，所设计的特种金刚石钻头能钻进 4～6

级可钻性的各种岩样，且钻头切削齿的温度仍在正常

范围内。这是自 2012 年 12 月正式启动了该原理样机

研制工作以来取得的重要进展，对于推动小行星深空

探测任务具有重要的意义。3）不断深化小行星深空

探测科学目标与有效载荷论证工作，组织了有机组分

仪器研制研讨会等会议。在第一届小行星探测学术研

讨会上作《中国未来小行星空间任务的任务概念》的

大会特邀报告，积极推动我国小行星深空探测任务。

（c）目标小天体形状建模研究：我们对小行星

探测任务中的目标小行星开展了科学研究。根据目前

观测给出的 14 条光变曲线，利用光变曲线反演程序，

得到 1996 FG3 的三维形状模型。重建的形状与雷达

观测获得的图像存在相似之处。该项工作还进一步确

定了该小行星的自转周期和指向范围。

2）小行星热物理模型研究方面：基于热物理模

型，利用数值模拟研究了近地小行星 1996 FG3 和

1999 JU3 的表面平均热惯量、反照率、有效直径、粗

糙度等物理性质，据此推测了小行星的表面特性，

1996 FG3 主星表面可能覆盖着一层颗粒很小的松散

物质，称之为风化层，其平均厚度大约为 5~20 mm(图

7) (Yu, Ji & Wang, 2013, MNRAS, submitted)；1999

JU3 表面绝大部分区域由岩石碎末或细沙等松散物质

覆盖 (余亮亮等，2013, 天文学报), 部分区域可能是

粗沙和石头的混合物, 极少的区域覆盖着较大的岩石

(图 8)。

3）系外行星研究方面：

（a）行星形成演化：研究了系外行星共振构型

的形成机制。根据目前 Kepler 发现的系外行星统计结

果，多行星系统中两颗行星处于 3:2 和 2:1 共振的较

多，其中处于 2:1 共振约为 16%，而 3:2 共振的比例

则更高。我们采用统计方法分别考虑了恒星吸积率、

恒星磁场强度以及第一类轨道迁移的速度对系外行

星中共振构型的形成影响，估计第一类轨道迁移速度

的合理范围，恒星磁场强弱，可以进一步估计行星形

成时所处的物理环境，为流体模拟提供了理论支持。

利用 N 体数值模拟方法研究了一个典型的分层

结构的双行星系统 Kepler-10 的潮汐演化。在动力学


18

模型中，我们主要考虑了中心恒星作用到内行星上的

潮汐效应和相对论效应，以及两颗行星之间的引力摄

动。模拟结果表明潮汐效应对该系统内行星形成的重

要作用，探讨了两颗行星的可能形成机制，内行星在

潮汐演化之前或许经历了行星之间的散射过程；外行

星可能经历了在原行星盘中的迁移过程（Dong & Ji,

2013, MNRAS）。

基于一般长期摄动理论研究了具有两颗行星的

数个 Kepler 行星系统在相互引力摄动、相对论效应以

及潮汐摄动作用下的轨道演化过程，获得了该类双行

星系统潮汐演化的一般图像，初步探讨了系统中潮汐

效应和引力效应的耦合作用。以 KOI 1239 系统为例，

结果表明潮汐效应的耗散项在轨道演化过程中起着

主导作用，而潮汐效应的保守项和恒星产生的相对论

效应将抑制行星在其它伴星长期摄动下的偏心率激

发（董瑶 & 季江徽, 2013，天文学报）。

利用数值模拟方法对 Vega 系统的碎片盘和可能

存在的行星进行了研究。在合理的初始假设下，通过

计算发现，若 Vega 系统中不存在行星，则碎片盘演

化结果与最新的观测结果吻合得较好；若系统中存在

行星，且行星偏心率较大（比如 e=0.6）时，则行星

的轨道半长轴不能大于 60 AU，否则碎片盘会在行星

的影响下产生明显的聚集现象，行星与碎片盘的 2:1

平运动共振是导致碎片盘产生结构的主要原因（Lu

& Ji，2013，Chin. Astron. and Astrophy.）。

（b）行星大气：研究了大气逃逸对系外行星的

影响。计算结果表明，小质量的行星对气体逃逸比较

敏感，而气态巨行星只能丢失很小一部分的初始大气。

大气逃逸能使行星族群产生一个位于 1 ～ 4 个地球

半径的双峰分布。大气逃逸可以把小质量行星的大气

完全剥离。对于这些只剩固态内核的行星，它们的半

径远小于那些还拥有一部分大气的行星。因此在整个

行星族群的半径分布图上，在 2 个地球半径附近产生

了一个空白区，把拥有部分大气的行星与失去全部大

气后只剩固态内核的行星分隔开来。

（c）行星内部结构：利用改进计算程序，研究

了具有大气的行星内部结构。

三、学术交流与合作

1. 国际合作与交流概况

2013 年紫台全年出访申请 158 人次（110 项，84

人，其中有 12 人次赴中国台湾地区访问），完成出访

任务 147 人次（其中中国台湾地区 11 人次），涉及 26

个国家/地区，出访形式主要包括所级协议合作研究

（62 人次）和国际会议（77 人次）等，出访国家/地

区以美国（34 人次）、德国（18 人次）、中国香港（14

人次）等为主。出访活动中，国际会议大会报告、分

会报告或墙报等 49 人次。全年来访 127 人次（63 项，

121 人），涉及 16 个国家/地区，主要包括院级国际合

作人才交流项目、科研合作和在华举办国际学术会议

等。与其他国家/地区人员合作发表论文 56 篇。

2013 年，紫台执行与国外研究机构和大学签订国

际合作协议 9 项，其中新增 4 项。人才培养方面，执

行中欧联合培养博士研究生 6 人，其中 2013 年新增 2

人，公派留学 2 项。国际合作（人才）项目方面，执

行“爱因斯坦讲席教授”1 项、“外国专家特聘研究员

计划”2 项、“外籍青年科学家计划”1 项，完成国际

合作重点项目 1 项。主办/承办的国际会议共 6 场，分

别是“第 13 届东亚地区亚毫米波接收机技术研讨会”、

“日球中高能粒子的探测和研究”、“东亚核心天文台

（EACOA）中等口径望远镜科学讨论会”、“高能天

体物理：亚洲天文学家培优学校的 COSPAR 能力建设

研讨会”、“第 2 届南极巡天望远镜合作会议”和“第

10 届中澳科技研讨会——天文与天体物理”。

2. 国际合作项目进展

1) 暗物质粒子探测合作研究

紫台主导的 A 类先导专项项目“暗物质粒子探测

卫星（DAMPE）”的硅微条的研制工作通过与瑞士日

内瓦大学的国际合作进行。2013 年，与瑞士日内瓦大

学就相关国际合作实施方案、技术流程、计划流程以

及应对估计合作风险等预案，硅微条与载荷其他分系

统、载荷总体及卫星总体的机械、电子学和热的接口

设计，研制样机的验收及相关试验等多个方面开展了

深入的讨论与合作研究。

与日本早稻田大学联合申请了国家自然科学基

金委与日本学术振兴会（JSPS）之间的中日科学合作

项目，重点对宇宙线进行科学观测方面的合作。双方

针对观测仪器设计、观测信号读出元器件选型、闪烁

晶体物理性能测试、探测总体结构设计、探测器物理

模拟仿真等方面进行了深入的研究与讨论。

南极天文合作研究


19

在国家极地科学考察的支持下，南极天文中心与

澳大利亚新南威尔士大学合作在南极冰穹 A 成功运

行南极巡天望远镜（AST3）并获得科学数据。2013

年 11 月，紫台组织中澳双方相关专家分别针对 AST3

和南极天文台 5 米太赫兹望远镜（DATE5）望远镜科

学目标和关键技术等开展了专题讨论，并深入研讨了

双方在南极天文方面进一步合作的前景和具体方案。

代表国家相关部门开展空间碎片等国际交流与

合作

紫金山天文台代表以国家航天局的名义参加了

2013 年 2 月在奥地利维也纳举办的联合国外空委科

技小组委员会第 50 届会议，与各国代表围绕“主动

碎片移除的技术”和“国际小行星预警网络与相应机

制”这两个热点议题进行了讨论交流；以中国国家航

天局的名义参加了 2013 年 4 月在德国达姆施塔特召

开的第 31 届机构间空间碎片协调委员会（IADC）会

议第一组（测量组，WG1）的会议，提交了 1 篇会议

报告，参加了会议讨论，表达了我国在有关议题上的

观点；2013 年 10-11 月，代表中国国家航天局参加了

IADC 组织的欧空局 GOCE 卫星陨落期预报国际联测

活动，目前正在进行中；2013 年下半年，代表中国国

家航天局参加了 IADC 组织的“大质量低轨目标反射

信号变化测量（光学部分）”国际联测活动，目前正

在进行中。

银河系结构和分子云与恒星形成系列合作研究

继续与德国马普射电天文所（MPIfR）和美国哈

佛史密松天体物理中心（CfA）等联合开展大型国际

合作计划——银河系棒和旋臂结构巡天（BeSSeL），

利用美国甚长基线干涉阵（VLBA）等设备首次实现

银河系本地臂的高精度测量，发现本地臂是形态和运

动学性质类似于其他主旋臂的一条独立旋臂，而非主

旋臂的分叉，引起国际广泛关注。

与 CfA 和 MPIfR 等合作，获得国际先进望远镜

SMA、APEX-10m、IRAM-30m、MPIfR-100m 等的观

测时间，开展银河系与星系中分子云与恒星形成的系

列观测研究工作。通过 SMA 的毫米波与亚毫米波连

续谱观测，领导完成国际上最大样本的高空间分辨率

原恒星巡天。通过统计发现：约有三分之二的原恒星

是双星或多星系统。该结果表明，双星形成模式是小

质量恒星形成的主要模式。

2) 太赫兹天文探测技术合作研究

通过法国国家科学研究中心 2013 年国际科研合

作项目（PICS）支持，与法国巴黎天文台毫米波

（LERMA）合作开展太赫兹超导热电子混频器探测

技术和太赫兹超导探测技术的合作研究。

与俄罗斯莫斯科师范大学（MSPU）和俄罗斯科

学院无线电工程和电子学研究所（IREE）合作，研制

太赫兹超导热电子探测器，联合开展了太赫兹超导热

电子混频器实验，在超导热电子探测器研制方面积累

了经验。

与日本理化学研究所（RIKEN）开展关于超导动

态电感探测器的合作研究，签署了双方合作协议，

2013 年 11 月访问 RIKEN，合作研究取得显著进展。

3) 太阳物理合作研究

年内民用航天预研项目“中法合作太阳爆发探测

小卫星（SMESE)中方有效载荷总体设计”通过院重

大科技任务局组织的项目结题验收。

完成院国际合作重点项目《莱曼α轨道望远镜

（LYOT）样机关键技术合作研究》。联合南京天文光

学技术研究所合作，与美国高山天文台联合开展地基

大口径日冕仪的光机联合设计，在南京召开科学目标

和关键技术研讨会，并签署联合研制谅解备忘录。

与意大利、德国同行多次联系，共同提出

ESA-CAS 联合空间科学卫星 SEEPE 提案，参与

2014-2015 年的项目遴选。

执行基金委中俄合作项目，年内邀请俄罗斯科学

院空间科学研究所等 5 人次来访，并 3 人次回访，针

对太阳耀斑能量及高能多波段辐射开展合作研究。

4) 星系形成合作研究

基于中德马普伙伴小组，继续与德国马普天文所

合作。本年度合作研究了温暗物质下的星系形成过程，

发现可以利用近邻星系的旋转曲线和恒星质量关系

来限制温暗物质的质量；研究了卫星星系的潮汐剥离

过程，指出卫星星系的物质剥离过程与其形态有紧密

联系；研究了冷气体吸积的稳定性问题，发现次并合

不能改变冷气体吸积的稳定性。


20

ABSTRACT LIST OF PUBLICATIONS IN 2013

Annual Report’2013–Abstract List of Publications in 2013

21

I. Dark Matter & Space Astronomy

Record 1 of 247

New constraints on anisotropic rotation of CMB polarization

Li, Mingzhe; Yu, Bo

Journal of Cosmology and Astroparticle Physics

期: 6; 页: 1-13

The coupling of a scalar field to electromagnetic field via the Chern-Simons term will rotate the polarization directions of the cosmic microwave background radiation. The rotation angle which relies on the distribution of the scalar field on the CMB sky is direction dependent. Such anisotropies will give rise to new distortions to the power spectra of CMB polarization and it can be used to probe the detailed physics of the scalar field. In this paper we use the updated observational data to constrain the anisotropic rotation angle in a model independent way. We find that the dominant effect of the anisotropic rotation on CMB comes from its variance and it is constrained tightly by the current data.

Record 2 of 247

Contribution of ultracompact dark matter minihalos to the isotropic radio background

Yang, Yupeng; Yang, Guilin; Huang, Xiaoyuan; Chen, Xuelei; Lu, Tan; Zong, Hongshi

PHYSICAL REVIEW D

卷: 87; 期: 8; 页: 083519-1-083519-6

The ultracompact minihalos could be formed during the earlier epoch of the Universe. The dark matter annihilation within them is very strong due to the steep density profile, rho similar to r(-2.25). The high-energy electrons and positrons from the dark matter annihilation can inverse Compton scatter with the background photons, such as cosmic microwave background photons, to acquire higher energy. On the other hand, the synchrotron radiation can also be produced when

they meet the magnetic field. In this paper, we study the signals from the ultracompact minihalos (UCMHs) due to the dark matter annihilation for the radio, x-ray and gamma-ray band. We found that for the radio emission, the UCMHs can provide one kind of source for the radio excess observed by ARCADE 2. But the x-ray signals due to the inverse Compton scatter effect or the gamma-ray signals mainly due to the prompt emission from dark matter would exceed the present observations, such as Fermi, COMPTEL, and CHANDRA. We found that the strongest limits on the fraction of UCMHs come from the x-ray observations, and the constraints from the radio data are the weakest.

Record 3 of 247

Impact of the local void on the cosmological parameters

Yu, Bo

JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS

期: 3; 页: 1-18

In this paper, I discuss the effects of a local void on the cosmological parameters. It is found that, if the supernova distance is absolutely calibrated, then the bias of all the cosmological parameters is always important, while if the supernova distance is relatively calibrated, the largest effects will appear in the dark energy equation of state. For a local void of size similar to 100Mpc, the bias effects mainly manifest in the low redshift range. Therefore, the piecewise dark energy equation of state, especially the one in the range of lowest redshift, will be more strongly affected than the constant equation of state. In order to reduce this bias in constraining the cosmological parameters, one could require the distance of all the adopted supernovas be greater than 1.2 similar to 1.5 times of the radius of the local void. In this case, the residual bias can be safely ignored.

Record 4 of 247

Cosmology, Dark Matter and High-Energy

Astrophysics


22

The relation between Pauli and gamma representation in QED(3) and induced Chern-Simons term

Shi Song ; Sun WeiMin; Zong HongShi

CHINESE SCIENCE BULLETIN

卷:58;期:31;页: 3735-3737

In this letter, we propose to introduce a new Abelian gauge field B (mu) corresponding to the so-called beta symmetry into the normal Quantum Electrodynamics in 2+1 dimensions (QED(3)) of gamma representation. The resulting theory is shown to be equivalent to QED(3) containing two flavors of two-component fermions with mass of an opposite sign. We also show that B (mu) field can generate a Chern-Simons term in perturbation theory. A comparison is made between the induced Chern-Simons term in the gamma representation and that in Pauli representation.

Record 5 of 247

Dust extinctions for an unbiased sample of gamma-ray burst afterglows

Covino, S.; Melandri, A.; Salvaterra, R.; Campana, S.; Vergani, S. D.; Bernardini, M. G.; D'Avanzo, P.; D'Elia, V.; Fugazza, D.; Ghirlanda, G.; Ghisellini, G.; Gomboc, A.; Jin, Z. P.; Kruhler, T.; Malesani, D.; Nava, L.; Sbarufatti, B.; Tagliaferri, G.

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY

卷: 432; 期: 2; 页: 1231-1244

In this paper, we compute rest-frame extinctions for the afterglows of a sample of Swift gamma-ray bursts (GRBs) complete in redshift. The selection criteria of the sample are based on observational high-energy parameters of the prompt emission and therefore our sample should not be biased against dusty sight-lines. It is therefore expected that our inferences hold for the general population of GRBs. Our main result is that the optical/near-infrared extinction of GRB afterglows in our sample does not follow a single distribution. 87 per cent of the events are absorbed by less than 2 mag, and 50 per cent suffer from less than 0.3-0.4 mag extinction. The remaining 13 per cent

of the afterglows are highly absorbed. The true percentage of GRB afterglows showing high absorption could be even higher since a fair fraction of the events without reliable redshift measurement are probably part of this class. These events may be due to highly dusty molecular clouds/star-forming regions associated with the GRB progenitor or along the afterglow line of sight, and/or due to massive dusty host galaxies. No clear evolution in the dust extinction properties is evident within the redshift range of our sample, although the largest extinctions are at z similar to 1.5-2, close to the expected peak of the star formation rate. Those events classified as dark are characterized, on average, by a higher extinction than typical events in the sample. A correlation between optical/near-infrared extinction and hydrogen-equivalent column density based on X-ray studies is shown, although the observed N-H appears to be well in excess compared to those observed in the Local Group. Dust extinction does not seem to correlate with GRB energetics or luminosity.

Record 6 of 247

GRB 081007 AND GRB 090424: THE SURROUNDING MEDIUM, OUTFLOWS, AND SUPERNOVAE

Jin, Zhi-Ping; Covino, Stefano; Della Valle, Massimo; Ferrero, Patrizia; Fugazza, Dino; Malesani, Daniele; Melandri, Andrea; Pian, Elena; Salvaterra, Ruben; Bersier, David; Campana, Sergio; Cano, Zach; Castro-Tirado, Alberto J.; D'Avanzo, Paolo; Fynbo, Johan P. U.; Gomboc, Andreja; Gorosabel, Javier; Guidorzi, Cristiano; Haislip, Joshua B.; Hjorth, Jens; Kobayashi, Shiho; LaCluyze, Aaron P.; Marconi, Gianni; Mazzali, Paolo A.; Mundell, Carole G.; Piranomonte, Silvia; Reichart, Daniel E.; Sanchez-Ramirez, Ruben; Smith, Robert J.; Steele, Ian A.; Tagliaferri, Gianpiero; Tanvir, Nial R.; Valenti, Stefano; Vergani, Susanna D.; Vestrand, Thomas; Walker, Emma S.; Wozniak, Przemek

ASTROPHYSICAL JOURNAL

卷: 774; 期: 2; 页: 114-1-114-9

We discuss the results of the analysis of multi-wavelength data for the afterglows of GRB 081007 and GRB 090424, two bursts detected by Swift. One of them, GRB 081007, also shows a spectroscopically confirmed supernova, SN 2008hw, which resembles SN 1998bw in its absorption features, while the maximum magnitude may be fainter, up to 0.7 mag, than

Gamma-Ray Burst, Neutron Star and

relevant physics


23

observed in SN 1998bw. Bright optical flashes have been detected in both events, which allows us to derive solid constraints on the circumburst-matter density profile. This is particularly interesting in the case of GRB 081007, whose afterglow is found to be propagating into a constant-density medium, yielding yet another example of a gamma-ray burst (GRB) clearly associated with a massive-star progenitor which did not sculpt the surroundings with its stellar wind. There is no supernova component detected in the afterglow of GRB 090424, likely due to the brightness of the host galaxy, comparable to the Milky Way. We show that the afterglow data are consistent with the presence of both forward-and reverse-shock emission powered by relativistic outflows expanding into the interstellar medium. The absence of optical peaks due to the forward shock strongly suggests that the reverse-shock regions should be mildly magnetized. The initial Lorentz factor of outflow of GRB 081007 is estimated to be Gamma similar to 200, while for GRB 090424 a lower limit of Gamma > 170 is derived. We also discuss the prompt emission of GRB 081007, which consists of just a single pulse. We argue that neither the external forward-shock model nor the shock-breakout model can account for the prompt emission data and suggest that the single-pulse-like prompt emission may be due to magnetic energy dissipation of a Poynting-flux-dominated outflow or to a dissipative photosphere.

Record 7 of 247

The last three outbursts of H1743-322 observed by RXTE in its latest service phase

Zhou, J. N.; Liu, Q. Z.; Chen, Y. P.; Li, J.; Qu, J. L.; Zhang, S.; Gao, H. Q.; Zhang, Z.


卷: 431; 期: 3; 页: 2285-2293

After 2010, three outbursts of H1743-322 were detected by RXTE. We have carried out timing and spectral analysis of the data, emphasizing on the two with relatively complete evolution history presented in the RXTE/Proportional Counter Array observations. We then constitute an enlarged outburst sample for H1743-322 which allows us to investigate the spectral transitions in more details. We find that the spectral transitions to high-soft state constrain a region for four outbursts in hardness-intensity diagram. An extension of the region locates in the vicinity of the failed outburst

in 2008, and excludes it from a successful group. We therefore suggest that the failed outburst in 2008 may present the first almost successful outburst sample, which is important for modelling the outburst, especially upon the conditions required for transition to high-soft state.

Record 8 of 247

IS THE LATE NEAR-INFRARED BUMP IN SHORT-HARD GRB 130603B DUE TO THE LI-PACZYNSKI KILONOVA?

Jin, Zhi-Ping; Xu, Dong; Fan, Yi-Zhong; Wu, Xue-Feng; Wei, Da-Ming

ASTROPHYSICAL JOURNAL LETTERS

卷: 775; 期: 1; 页: L19-1-L19-4

Short-hard gamma-ray bursts (GRBs) are widely believed to be produced by the merger of two binary compact objects, specifically by two neutron stars or by a neutron star orbiting a black hole. According to the Li-Paczynski kilonova model, the merger would launch sub-relativistic ejecta and a near-infrared/optical transient would then occur, lasting up to days, which is powered by the radioactive decay of heavy elements synthesized in the ejecta. The detection of a late bump using the Hubble Space Telescope (HST) in the near-infrared afterglow light curve of the short-hard GRB 130603B is indeed consistent with such a model. However, as shown in this Letter, the limited HST near-infrared light curve behavior can also be interpreted as the synchrotron radiation of the external shock driven by a wide mildly relativistic outflow. In such a scenario, the radio emission is expected to peak with a flux of similar to 100 mu Jy, which is detectable for current radio arrays. Hence, the radio afterglow data can provide complementary evidence on the nature of the bump in GRB 130603B. It is worth noting that good spectroscopy during the bump phase in short-hard bursts can test the validity of either model above, analogous to spectroscopy of broad-lined Type Ic supernova in long-soft GRBs.

Record 9 of 247

Cosmological Time Dilation in Durations of Swift Long Gamma-Ray Bursts

Zhang, Fu-Wen; Fan, Yi-Zhong; Shao, Lang; Wei, Da-Ming


卷: 778; 期: 1; 页: L11-1-L11-5

Cosmological time dilation is a fundamental phenomenon in an expanding universe, which


24

stresses that both the duration and wavelength of the emitted light from a distant object at the redshift z will be dilated by a factor of 1 + z at the observer. By using a sample of 139 Swift long gamma-ray bursts with known redshift (z <= 8.2), we measure the observed duration (T-90) in the observed energy range between 140/(1 + z) keV and 350/(1 + z) keV, corresponding to a fixed energy range of 140-350 keV in the rest frame. We obtain a significant correlation between the duration and the factor 1 + z, i.e., T-90 = 10.5(1 + z) (0.94 +/- 0.26), which is consistent with that expected from the cosmological time dilation effect.

Record 10 of 247

Multi-wavelength Study of the Be/X-ray Binaries

Yan, J. Z.; Li, H.; Zhou, J. N.; Liu, Q. Z.

IAU Symposium

卷: 290; 页: 351-352

An anti-correlation between the optical brightness and the strength of the Hα emission was observed from two Be/X-ray binaries, A0535+26 and MXB 0656-072: when the optical brightness showed a decrease, the intensity of the Hα emission displayed an obvious increase. This anti-correlation is interpreted as the result of the mass ejection from the Be star. After the mass ejection event, a cavity or low-density region will be developing in the inner parter of the circumstellar disk. The X-ray outbursts of the Be/X-ray binaries might be connected with the mass ejections from the Be star.

Record 11 of 247

2D and 3D Polar Plume Analysis from the Three Vantage Positions of STEREO/EUVI A, B, and SOHO/EIT

de Patoul, Judith; Inhester, Bernd; Feng, Li; Wiegelmann, Thomas

SOLAR PHYSICS

卷: 283; 期: 1; 页: 207-225

Polar plumes appear as elongated objects starting at the solar polar regions. Here we analyze these objects from a sequence of images taken simultaneously by the three spacecraft telescopes STEREO/EUVI A and B, and SOHO/EIT. We

establish a method capable of automatically identifying plumes in solar EUV images close to the limb at 1.01 -aEuro parts per thousand 1.39 R (aS (TM)) in order to study their temporal evolution. This plume-identification method is based on a multiscale Hough-wavelet analysis. Then two methods to determine the 3D localization and structure of the plumes are discussed: first, tomography using filtered back-projection and including the differential rotation of the Sun and, second, conventional stereoscopic triangulation. We show that tomography and stereoscopy are complementary for studying polar plumes. We also show that this systematic 2D identification and the proposed methods of 3D reconstruction are well suited to identify plumes individually and also to analyze the distribution of plumes and inter-plume regions. Finally, the results are discussed, focusing on plume position and cross-sectional area.

Record 12 of 247

Observations of a Quasi-periodic, Fast-Propagating Magnetosonic Wave in Multiple Wavelengths and Its Interaction with Other Magnetic Structures

Shen, Y. -D.; Liu, Y.; Su, J. -T.; Li, H.; Zhang, X. -F.; Tian, Z. -J.; Zhao, R. -J.; Elmhamdi, A.

SOLAR PHYSICS

卷: 288; 期: 2; 页: 585-602

We present observations of a quasi-periodic fast-propagating (QFP) magnetosonic wave on 23 April 2012, with high-resolution observations taken by the Atmospheric Imaging Assembly onboard the Solar Dynamics Observatory. Three minutes after the start of a C2.0 flare, wave trains were first observed along an open divergent loop system in 171 observations at a distance of 150 Mm from the footpoint of the guiding loop system and with a speed of 689 km s(-1), then they appeared in 193 observations after their interaction with a perpendicular, underlaying loop system on the path; in the meantime; their speed decelerated to 343 km s(-1) within a short time. The sudden deceleration of the wave trains and their appearance in 193 observations are interpreted through a geometric effect and the density increase of the guiding loop system, respectively. We find that the wave trains have a common period of 80 seconds with the flare. In addition, a few low frequencies are also identified in the QFP wave. We propose that the generation

High-Energy Solar Astrophysics


25

of the period of 80 seconds was caused by the periodic releasing of energy bursts through some nonlinear processes in magnetic reconnection, while the low frequencies were possibly the leakage of pressure-driven oscillations from the photosphere or chromosphere, which could be an important source for driving coronal QFP waves. Our results also indicate that the properties of the guiding magnetic structure, such as the distributions of magnetic field and density as well as geometry, are crucial for modulating the propagation behaviors of QFP waves.

Record 13 of 247

ELECTRON AND PROTON ACCELERATION DURING THE FIRST GROUND LEVEL ENHANCEMENT EVENT OF SOLAR CYCLE 24

Li, C.; Firoz, Kazi A.; Sun, L. P.; Miroshnichenko, L. I.


卷: 770; 期: 1; 页: 34-1-34-11

High-energy particles were recorded by near-Earth spacecraft and ground-based neutron monitors (NMs) on 2012 May 17. This event was the first ground level enhancement (GLE) of solar cycle 24. In this study, we try to identify the acceleration source(s) of solar energetic particles by combining in situ particle measurements from the WIND/3DP, GOES 13, and solar cosmic rays registered by several NMs, as well as remote-sensing solar observations from SDO/AIA, SOHO/LASCO, and RHESSI. We derive the interplanetary magnetic field (IMF) path length (1.25 +/- 0.05 AU) and solar particle release time (01: 29 +/- 00: 01 UT) of the first arriving electrons by using their velocity dispersion and taking into account contamination effects. We found that the electron impulsive injection phase, indicated by the dramatic change in the spectral index, is consistent with flare non-thermal emission and type III radio bursts. Based on the potential field source surface concept, modeling of the open-field lines rooted in the active region has been performed to provide escape channels for flare-accelerated electrons. Meanwhile, relativistic protons are found to be released similar to 10 minutes later than the electrons, assuming their scatter-free travel along the same IMF path length. Combining multi-wavelength imaging data of the prominence eruption and coronal mass ejection (CME), we obtain evidence that GLE protons, with an estimated kinetic energy of similar to 1.12 GeV, are probably accelerated by the CME-driven shock

when it travels to similar to 3.07 solar radii. The time-of-maximum spectrum of protons is typical for shock wave acceleration.

Record 14 of 247

Imaging coronal magnetic-field reconnection in a solar flare

Su, Yang; Veronig, Astrid M.; Holman, Gordon D.; Dennis, Brian R.; Wang, Tongjiang; Temmer, Manuela; Gan, Weiqun

NATURE PHYSICS

卷: 9; 期: 8; 页: 489-493

Magnetic-field reconnection is believed to play a fundamental role in magnetized plasma systems throughout the Universe(1), including planetary magnetospheres, magnetars and accretion disks around black holes. This letter presents extreme ultraviolet and X-ray observations of a solar flare showing magnetic reconnection with a level of clarity not previously achieved. The multi-wavelength extreme ultraviolet observations from SDO/AIA show inflowing cool loops and newly formed, outflowing hot loops, as predicted. RHESSI X-ray spectra and images simultaneously show the appearance of plasma heated to >10MK at the expected locations. These two data sets provide solid visual evidence of magnetic reconnection producing a solar flare, validating the basic physical mechanism of popular flare models. However, new features are also observed that need to be included in reconnection and flare studies, such as three-dimensional non-uniform, non-steady and asymmetric evolution.

Record 15 of 247

Error Assessment in Modeling with Fractal Brownian Motions

QIAO, BINGQIANG; LIU SIMING

FRACTALS

卷: 21; 期: 4; 页: 1-6

To model a given time series F(t) with fractal Brownian motions (fBms), it is necessary to have appropriate error assessment for related quantities. Usually the fractal dimension D is derived from the Hurst exponent H via the relation D = 2-H, and the Hurst exponent can be evaluated by analyzing the dependence of the rescaled

range 〈|F(t + τ) - F(t)|〉 on the time span τ. For fBms, the error of the rescaled range not only depends on data sampling but also varies with H due to the presence of long term memory. This

http://libir.pmo.ac.cn/simple-search?query1=FRACTALS&field1=source&advanced=false


26

error for a given time series then can not be assessed without knowing the fractal dimension. We carry out extensive numerical simulations to explore the error of rescaled range of fBms and find that for 0 < H < 0.5, |F(t + τ) - F(t)| can be treated as independent for time spans without overlap; for 0.5 < H < 1, the long term memory makes |F(t + τ) - F(t)| correlated and an approximate method is given to evaluate the error

of 〈|F(t + τ) - F(t)|〉. The error and fractal

dimension can then be determined self-consistently in the modeling of a time series with fBms.

Record 16 of 247

The breakdown of the power-law frequency distributions for the hard X-ray peak count rates of solar flares

Li, You-Ping; Gan, Wei-Qun; Feng, Li; Liu, Si-Ming; Struminsky, A.

RESEARCH IN ASTRONOMY AND ASTROPHYSICS

卷: 13; 期: 12; 页: 1482-1492

The frequency distribution for several characteristics of a solar flare obeys a power law only above a certain threshold, below which there is an apparent loss of small scale events presumably caused by limited instrumental sensitivity and the corresponding event selection bias. It is also possible that this deviation in the power law can have a physical origin in the source. We propose two fitting models incorporating a power law distribution with a low count rate cutoff plus a noise component for the frequency distribution of the hard X-ray peak count rate of all solar flare samples obtained with HXRBS/SMM and BATSE/CGRO observations. Our new fitting method produces the same power-law index as previously developed methods, a low cutoff of the power-law function and its corresponding noise level, which is consistent with measurements of the actual noise level of the hard X-ray count rate. We found that the fitted low cutoff appears to be related to the noise level, i.e., flares are only recognized when their peak count rate is 3 sigma greater than noise. Therefore, the fitted low cutoff, which is smaller than the aforementioned threshold, might be attributed to selection bias, and probably not to the actual count rate cutoff in flares at smaller scales. Whether or not the actual low cutoff physically exists needs to be checked by future observations with increased sensitivities.

Record 17 of 247

Comparisons of CME Morphological Characteristics Derived from Five 3D Reconstruction Methods

Feng, L.; Inhester, B.; Mierla, M.

SOLAR PHYSICS

卷: 282; 期: 1; 页: 221-238

We compare different methods to reconstruct three-dimensional (3D) coronal mass ejection (CME) morphology. The explored methods include geometric localisation, mask fitting, forward modelling, polarisation ratio, and local correlation tracking plus triangulation. These five methods are applied to the same CME event that occurred on 7 August 2010. Their corresponding results are presented and compared, especially in their propagation direction and spatial extent in 3D. We find that the mask fitting and geometric localisation methods produce consistent results. Reconstructions including three-view observations are more precise than reconstructions done with only two views. Compared to the forward modelling method, in which an a priori shape of the CME geometry is assumed, the mask fitting has more flexibility. The polarisation ratio method makes use of the Thomson scattering geometry. We find that spatially the 3D CME derived from the mask fitting lies mostly in the overlap region obtained with the polarisation method using data from STEREO. In addition, the mask fitting can help resolve the front/back ambiguity inherent in the polarisation ratio method. However, the local correlation tracking plus triangulation did not show consistent results with the other four methods. This method performed poorly, primarily because the two STEREO spacecraft had a large angular separation. Under these circumstances, it is difficult to identify points taken from independent images that correspond to the same physical feature. Excluding the local correlation tracking method, the latitude of the CME's centre of gravity derived from the other methods deviates within 1(a similar to), and the longitude differs within 19 degrees.

Record 18 of 247

HIGH-z QUASARS IN THE R-h = ct UNIVERSE

Melia, Fulvio


卷: 764; 期: 1; 页: 72-1-72-5

One cannot understand the early appearance of 10(9)M(circle dot) supermassive black holes without invoking anomalously high accretion rates or the creation of exotically massive seeds, neither


27

of which is seen in the local universe. Recent observations have compounded this problem by demonstrating that most, if not all, of the high-z quasars appear to be accreting at the Eddington limit. In the context of Lambda CDM, the only viable alternative now appears to be the assemblage of supermassive black holes via mergers, as long as the seeds started forming at redshifts > 40, but ceased being created by z similar to 20-30. In this paper, we show that, whereas the high-z quasars may be difficult to explain within the framework of the standard model, they can instead be interpreted much more sensibly in the context of the R-h = ct universe. In this cosmology, 5-20 M-circle dot seeds produced after the onset of re-ionization (at z less than or similar to 15) could have easily grown to M greater than or similar to 10(9) M-circle dot by z greater than or similar to 6, merely by accreting at the standard Eddington rate.

Record 19 of 247

ENERGY PARTITION BETWEEN ENERGETIC ELECTRONS AND TURBULENT MAGNETIC FIELD IN SUPERNOVA REMNANT RX J1713.7-3946

Yang, Chuyuan; Liu, Siming


卷: 773; 期: 2; 页: 138-1-138-6

Current observations of supernova remnant (SNR) RX J1713.7-3946 favor the leptonic scenario for the TeV emission, where the radio to X-ray emission is produced via the synchrotron process and the gamma-ray emission is produced via the inverse Comptonization of soft background photons, and the electron distribution can be inferred from the observed gamma-ray spectrum with a spectral inversion method. It is shown that the observed correlation between the X-ray and gamma-ray brightness of SNR RX J1713.7-3946 can be readily explained with the assumption that the energy density of energetic electrons is proportional to that of the magnetic field in such a scenario. A two-dimensional magnetohydrodynamic simulation is then carried out to model the overall emission spectrum. It is found that the total energy of electrons above similar to 1 GeV is equal to that of the magnetic field. This is the first piece of observational evidence for energy equipartition between energetic electrons and magnetic field in the downstream of strong collisionless astrophysical shocks of SNRs.

Record 20 of 247

MAGNETIC ENERGY PARTITION BETWEEN THE CORONAL MASS EJECTION AND FLARE FROM AR 11283

Feng, L.; Wiegelmann, T.; Su, Y.; Inhester, B.; Li, Y. P.; Sun, X. D.; Gan, W. Q.


卷: 765; 期: 1; 页: 37-1-37-11

On 2011 September 6, an X-class flare and a halo coronal mass ejection (CME) were observed from Earth erupting from the same active region AR 11283. The magnetic energy partition between them has been investigated. SDO/HMI vector magnetograms were used to obtain the coronal magnetic field using the nonlinear force-free field (NLFFF) extrapolation method. The free magnetic energies before and after the flare were calculated to estimate the released energy available to power the flare and the CME. For the flare energetics, thermal and nonthermal energies were derived using the RHESSI and GOES data. To obtain the radiative output, SDO/EVE data in the 0.1-37 nm waveband were utilized. We have reconstructed the three-dimensional (3D) periphery of the CME from the coronagraph images observed by STEREO-A, B, and SOHO. The mass calculations were then based on a more precise Thomson-scattering geometry. The subsequent estimate of the kinetic and potential energies of the CME took advantage of the more accurate mass, and the height and speed in a 3D frame. The released free magnetic energy resulting from the NLFFF model is about 6.4x10(31) erg, which has a possible upper limit of 1.8x10(32) erg. The thermal and nonthermal energies are lower than the radiative output of 2.2x10(31) erg from SDO/EVE for this event. The total radiation covering the whole solar spectrum is probably a few times larger. The sum of the kinetic and potential energy of the CME could go up to 6.5x10(31) erg. Therefore, the free energy is able to power the flare and the CME in AR 11283. Within the uncertainty, the flare and the CME may consume a similar amount of free energy.

Record 21 of 247

KELVIN-HELMHOLTZ INSTABILITY OF A CORONAL STREAMER

Feng, L.; Inhester, B.; Gan, W. Q.



28

卷: 774; 期: 2; 页: 141-1-141-9

Shear-flow-driven instability can play an important role in energy transfer processes in coronal plasma. We present for the first time the observation of a kink-like oscillation of a streamer that is probably caused by the streaming kink-mode Kelvin-Helmholtz instability (KHI). The wave-like behavior of the streamer was observed by the Large Angle and Spectrometric Coronagraph Experiment C2 and C3 on board the SOlar and Heliospheric Observatory. The observed wave had a period of about 70-80 minutes, and its wavelength increased from 2 R-circle dot to 3 R-circle dot in about 1.5 hr. The phase speeds of its crests and troughs decreased from 406 +/- 20 to 356 +/- 31 km s(-1) during the event. Within the same heliocentric range, the wave amplitude also appeared to increase with time. We attribute the phenomena to the MHD KHI, which occurs at a neutral sheet in a fluid wake. The free energy driving the instability is supplied by the sheared flow and sheared magnetic field across the streamer plane. The plasma properties of the local environment of the streamer were estimated from the phase speed and instability threshold criteria.

Record 22 of 247

Impulsive Thermal X-Ray Emission from a Low-lying Coronal Loop

Liu, Siming; Li, Youping; Fletcher, Lyndsay


卷: 769; 期: 2; 页: 135-1-135-10

Understanding the relationship among different emission components plays an essential role in the study of particle acceleration and energy conversion in solar flares. In flares where gradual and impulsive emission components can be readily identified, the impulsive emission has been attributed to non-thermal particles. We carry out detailed analysis of H alpha and X-ray observations of a GOES class B microflare loop on the solar disk. The impulsive hard X-ray emission, however, is found to be consistent with a hot, quasi-thermal origin, and there is little evidence of emission from chromospheric footpoints, which challenges conventional models of flares and reveals a class of microflares associated with dense loops. H alpha observations indicate that the loop lies very low in the solar corona or even in the chromosphere and both emission and absorption materials evolve during the flare. The enhanced H alpha emission may very well originate from the photosphere when the low-lying flare loop heats

up the underlying chromosphere and reduces the corresponding H alpha opacity. These observations may be compared with detailed modeling of flare loops with the internal kink instability, where the mode remains confined in space without apparent change in the global field shape, to uncover the underlying physical processes and to probe the structure of solar atmosphere.

Record 23 of 247

Parameters of the flare and surrounding medium and their evolution during 20 January 2005 solar event

Troitskaia, E.; Arkhangelskaja, I.; Arkhangelsky, A.; Gan, W.

Journal of Physics: Conference Series, 23rd European Cosmic Ray Symposium

卷: 409; 期: 1; 页: 012204-1-012204-9

Basing on the data of AVS-F apparatus from SONG-D detector onboard CORONAS-F satellite, we have studied the extreme solar event of January 20, 2005 used the 2.223 MeV, 4.44 MeV and 6.13 MeV -lines temporal profiles. By the statistical modeling method we calculated the temporal profile of 2.223 MeV line too. Calculations have been performed in assumption of Bessel type of accelerated particles energy spectrum, different 3He content in the region of nuclear reactions and several density models of the solar atmosphere. Comparisons of the results of modeling with observational 2.223 MeV AVS-F/SONG-D data reveal the increasing of the ratio of 3He concentration to 1H one during the flare from 2 10-5 at the rise phase of the gamma-ray flux up to 2 10- 4 at the decay one. During the same period the spectrum became harder and the density of solar atmosphere increased too. Averaged over full time of 2.223 MeV -emission concentration ratio of 3He/1H is equal to (1.400.15)10- 4, also the density model with enlarged density up to 21017 cm-3 in the lower chromosphere and through the whole photosphere is realized. Besides, we have estimated the spectral index T that is close to 0.1 for accelerated protons in the range of 1-100 MeV. Using the AVS-F gamma-rays spectral data in the wide range up to 140 MeV, we have obtained the spectral index of s=2.50.1 in the case of power law spectrum for energies more than 300 MeV.

Record 24 of 247


29

Polar jet kinetics and energetics analysed from STEREO/COR data

Feng, Li; Gan, Weiqun

Solar and Astrophysical Dynamos and Magnetic Activity, Proceedings of the International Astronomical Union, IAU Symposium

卷: 294; 页: 549-550

We analyze coronagraph observations of a polar jet eruption observed by SECCHI/STEREO. The brightness distribution of the jet in white-light coronagraph images is compared with a kinetic particle model. In this first application, we consider only gravity as the dominant force on the jet particles along the magnetic field. The kinetic model explains well the observed brightness evolution. The initial particle velocity distribution is fitted by Maxwellian distributions and we find deviations of the high energy tail from the Maxwellian distributions. The jets total mass is between 3.2×10

14 and 1.8×10

15 g. The total kinetic

energy of all the particles in the jet source region amounts from 2.1×10

28 to 2.4×10

29 ergs.

Record 25 of 247

Solar Flares with an Exponential Growth of the Emission Measure in the Impulsive Phase Derived from X-ray Observations

Han, Fei-ran; Liu, Siming

Chinese Astronomy and Astrophysics

卷: 37; 期: 3; 页: 277-293

The light curves of solar flares in the impulsive phase are complex in general, indicating that multiple physical processes are involved in. With the GOES (Geostationary Operational Environmental Satellite) observations, we find that there are a subset of flares, whose impulsive phases are dominated by a period of exponential growth of the emission measure. The flares occurred from January 1999 to December 2002 are analyzed, and the results from the observations made with both GOES 8 and GEOS 10 satellites are compared to estimate the instrumental uncertainties. Their mean temperatures during this exponential growth phase have a normal distribution. Most flares within the 1σ range of this temperature distribution belong to the GOES class B or C, with the peak fluxes at the GOES low-energy channel following a log-normal distribution. The growth rate and duration of the exponential growth phase also follow a log- normal distribution, in which the duration is distributed in the range from half a minute to about half an hour. As expected, the

growth time is correlated with the decay time of the soft X-ray flux. We also find that the growth rate of the emission measure is strongly anti-correlated with the duration of the exponential growth phase, and the mean temperature increases slightly with the increase of the growth rate. The implications of these results on the study of energy release in solar flares are discussed in the end.

Record 26 of 247

A Research on CdZnTe Array Detector

Cai Mingsheng; Guo Jianhua; Xie Minggang; Zheng Chunxiao

ACTA ASTRONOMICA SINICA

卷:54;期:5;页:467-477

The CdZnTe array detector is a new type of semiconductor detector, and it has been developing rapidly in recent years. It has some characteristics of high spatial resolution, high energy resolution, and it can work at room temperature. This article describes the physical characteristics and the working principle of the CdZnTe detector. It also introduces the production process of the CdZnTe array detector, including the pretreatment of the chips, passivation, ohmic electrode production, array template selection, and array package process selection (micro-interconnect). For evaluating the performance of the detector, the authors produced a 4 pixel x 4 pixel CdZnTe array and an 8 pixel x 8 pixel CdZnTe array (The thicknesses are 5 mm and 2 mm, respectively. The pixel size is 2 mm x 2 mm. The gaps are 0.15 mm and 0.2 mm, respectively.) with cooperation partner successfully. A multi-channel electronic readout system based on the ASIC (Application Specific Integrated Circuit) chip is used for the charge measurement of the 4 pixel x 4 pixel array of CdZnTe. The 16-pixel spectrum and the corresponding energy resolution are obtained with the ~(137)Cs radiation source. Among the results of each pixel, the best resolution is 4.8%@662 keV.

Record 27 of 247

Multi-Band Observation of Solar Activity


30

Ha Surges Aroused by Newly-emerging Satellite Bipolar Magnetic Field

Wang, Junfeng; Zhou, Tuanhui; Ji, Haisheng;


卷: 54; 期: 4; 页: 318-326

An Hαsurge event occurred at AR NOAA 11259 on 2011 July 22.According to the BBSO(Big Bear Solar Observatory) Hαline-center observations,three surges continuously ejected from the same region to the north of the main-sunspot of AR 11259. All of surges ejected along a straight trajectory,and looked like the reversed Eiffel Tower. The first and second surges had the same process.Two bright points firstly appeared to the north of the main-sunspot.After several minutes,a surge appeared between the two bright points,and then rapidly ejected when the two points got most brightness.When the surge reached the maximum height,it disappeared quickly.However,the third surge appeared without bright points,and its height was only half of the others.Compared with SDO/HMI ( Solar Dynamics Observatory/Helioseismic and Magnetic Imager ) line-of-sight magnetogram,more than one hour before the first surge appeared,a satellite bipolar magnetic field emerged from the surge-ejection region.The newly-emerging positive magnetic flux showed a distinct decrease several minutes earlier than the ejection of the surges.We assumed that the surges was associated with the reconnection between the newly-emerging bipolar magnetic field and the existing(sunspot) magnetic field.

Record 28 of 247

Recent advances in solar storm studies in China

Wang JingXiu; Ji HaiSheng

SCIENCE CHINA-EARTH SCIENCES

卷: 56; 期: 7; 页: 1091-1117

Solar storm has been commonly accepted by academic community and the public as a very popular scientific term. It is a vivid description of violent ejections of a huge amount of magnetized plasma from the Sun as strong flare/CMEs, which sweep over into interplanetary space, develop, and affect our space environment. The solar storm could bring us disastrous space weather, destroy crucial technology, and cause a large-scale blackout. It is one of the natural disasters faced by modern human beings. Here we first briefly summarize the observational features of solar storms and introduce some key issues, and then we focus on major advances in observational studies. We mainly introduce the efforts made by

the Chinese scientists and comment on the challenges and opportunities that they are facing. In this era when scientific breakthroughs in solar storm studies crucially depend on space-borne devices and large-aperture ground-based telescopes, the Chinese solar research community needs to develop its own major observational facilities and improve space weather forecasting abilities.

Record 29 of 247

Spatially Resolved Microwave Observations of Multiple Periodicities in a Flaring Loop

Kupriyanova, E. G.; Melnikov, V. F.; Shibasaki, K.

SOLAR PHYSICS

卷: 284; 期: 2; 页: 559-578

Quasi-periodic pulsations (QPPs) with at least three simultaneously existing spectral components with periods Pa parts per thousand yen30 s, Pa parts per thousand 20 s, and about Pa parts per thousand 10 s were detected during the decay phase of a solar flare on 3 July 2002, observed with the Nobeyama Radioheliograph (NoRH). A detailed study of the spatial structure of the Fourier amplitudes of QPPs along a flaring loop has revealed different spatial distributions of the three components. It is shown that the source of the QPPs with period Pa parts per thousand yen30 s has its maximum amplitude in the inner region of the loop, between the footpoints. QPPs with period Pa parts per thousand 20 s are localized at the periphery of the loop, mainly in the outer parts of the footpoints. The spatial distribution of oscillations with period about Pa parts per thousand 10 s contains three regions of high QPP amplitudes: two near the footpoints and one in the middle of the flaring region. It is shown that the observed properties of the spectral components are most accurately described by the fundamental, second, and third harmonics of the kink mode standing waves. This is the first identification of the kink mode in flare loops which is based on strict limitations derived from data on the spatial structure of a pulsating flare region.

Record 30 of 247

Parametric survey of longitudinal prominence oscillation simulations

Zhang, Q. M.; Chen, P. F.; Xia, C.; Keppens, R.; Ji, H. S.

ASTRONOMY & ASTROPHYSICS


31

卷: 554; 页: A124-1-A124-8

Context. Longitudinal filament oscillations recently attracted increasing attention, while the restoring force and the damping mechanisms are still elusive. Aims. We intend to investigate the underlying physics for coherent longitudinal oscillations of the entire filament body, including their triggering mechanism, dominant restoring force, and damping mechanisms. Methods. With theMPI-AMRVAC code, we carried out radiative hydrodynamic numerical simulations of the longitudinal prominence oscillations. We modeled two types of perturbations of the prominence, impulsive heating at one leg of the loop and an impulsive momentum deposition, which cause the prominence to oscillate. We studied the resulting oscillations for a large parameter scan, including the chromospheric heating duration, initial velocity of the prominence, and field line geometry. Results. We found that both microflare-sized impulsive heating at one leg of the loop and a suddenly imposed velocity perturbation can propel the prominence to oscillate along the magnetic dip. Our extensive parameter survey resulted in a scaling law that shows that the period of the oscillation, which weakly depends on the length and height of the prominence and on the amplitude of the perturbations, scales with root R/g(circle dot), where R represents the curvature radius of the dip, and g(circle dot) is the gravitational acceleration of the Sun. This is consistent with the linear theory of a pendulum, which implies that the field-aligned component of gravity is the main restoring force for the prominence longitudinal oscillations, as confirmed by the force analysis. However, the gas pressure gradient becomes significant for short prominences. The oscillation damps with time in the presence of non-adiabatic processes. Radiative cooling is the dominant factor leading to damping. A scaling law for the damping timescale is derived, i.e., tau similar to l(1.63)D(0.66)omega(-1.21)v(0)(-0.30), showing strong dependence on the prominence length l, the geometry of the magnetic dip (characterized by the depth D and the width w), and the velocity perturbation amplitude v(0). The larger the amplitude, the faster the oscillation damps. We also found that mass drainage significantly reduces the damping timescale when the perturbation is too strong.

Record 31 of 247

OBSERVATION OF MAGNETIC RECONNECTION DRIVEN BY GRANULAR SCALE ADVECTION

Zeng, Zhicheng; Cao, Wenda; Ji, Haisheng


卷: 769; 期: 2; 页: L33-1-L33-7

We report the first evidence of magnetic reconnection driven by advection in a rapidly developing large granule using high spatial resolution observations of a small surge event (base size similar to 4 '' x 4 '') with the 1.6 m aperture New Solar Telescope at the Big Bear Solar Observatory. The observations were carried out in narrowband (0.5 angstrom) He I 10830 angstrom and broadband (10 angstrom) TiO 7057 angstrom. Since He I 10830 angstrom triplet has a very high excitation level and is optically thin, its filtergrams enable us to investigate the surge from the photosphere through the chromosphere into the lower corona. Simultaneous space data from the Atmospheric Imaging Assembly and Helioseismic and Magnetic Imager on board the Solar Dynamics Observatory were used in the analysis. It is shown that the surge is spatio-temporally associated with magnetic flux emergence in the rapidly developing large granule. During the development of the granule, its advecting flow (similar to 2 km s(-1)) squeezed the magnetic flux into an intergranular lane area, where a magnetic flux concentration was formed and the neighboring flux with opposite magnetic polarity was canceled. During the cancellation, the surge was produced as absorption in He I 10830 angstrom filtergrams while simultaneous EUV brightening occurred at its base. The observations clearly indicate evidence of a finest-scale reconnection process driven by the granule's motion.

Record 32 of 247

Concerning spikes in emission and absorption in the microwave range

Chernov, Gennady P.; Sych, Robert A.; Huang, Guang-Li; Ji, Hai-Sheng; Yan, Yi-Hua; Tan, Cheng-Ming


卷: 13; 期: 1; 页: 115-128

In some events, weak fast solar bursts (near the level of the quiet Sun) were observed in the background of numerous spikes in emission and absorption. In such a case, the background contains the noise signals of the receiver. In events on 2005 September 16 and 2002 April 14, the solar origin of fast bursts was confirmed by


32

simultaneous recording of the bursts at several remote observatories. The noisy background pixels in emission and absorption can be excluded by subtracting a higher level of continuum when constructing the spectra. The wavelet spectrum, noisy profiles in different polarization channels and a spectrum with continuum level greater than zero demonstrates the noisy character of pixels with the lowest levels of emission and absorption. Thus, in each case, in order to judge the solar origin of all spikes, it is necessary to determine the level of continuum against the background of which the solar bursts are observed. Several models of microwave spikes are discussed. The electron cyclotron maser emission mechanism runs into serious problems with the interpretation of microwave millisecond spikes: the main obstacles are too high values of the magnetic field strength in the source (omega(Pe) <= omega(Be)). The probable mechanism is the interaction of plasma Langmuir waves with ion-sound waves (l + s -> t) in a source related to shock fronts in the reconnection region.

Record 33 of 247

The calculation of coronal magnetic field and density of nonthermal electrons in the 2003 October 27 microwave burst

Huang, Guang-Li; Li, Jian-Ping; Song, Qi-Wu


卷: 13; 期: 2; 页: 215-225

Based on Dulk and Marsh's approximate theory about nonthermal gyrosynchrotron radiation, one simple impulsive microwave burst with a loop-like structure is selected for radio diagnostics of the coronal magnetic field and column density of nonthermal electrons, which are calculated from the brightness temperature, polarization degree, and spectral index, as well as the turnover frequency, observed by using the Nobeyama Radioheliograph and the Nobeyama Radio Polarimeters, respectively. Very strong variations (up to one or two orders of magnitude) of the calculated transverse and longitudinal magnetic fields with respect to the line-of-sight, as well as the calculated electron column density, appear in the looptop and footpoint sources during the burst. The absolute magnitude and varied range of the transverse magnetic field are evidently larger than those of the longitudinal magnetic field. The time evolution of the transverse magnetic field is always anti-correlated with that of the longitudinal magnetic field, but positively

correlated with that of the electron column density. These results strongly support the idea that quantifying the energy released in a flare depends on a reconstruction of the coronal magnetic field, especially for the transverse magnetic field, and they are basically consistent with the recent theoretical and observational studies on the photospheric magnetic field in solar flares.

Record 34 of 247

Analysis of the coronal source of the partially limb-occulted flare on 2002 July 20

Shen, Jin-Hua; Melnikov, Victor; Zhou, Tuan-Hui; Ji, Hai-Sheng


卷: 13; 期: 8; 页: 961-977

We carry out a detailed analysis of the X3.5 solar flare that occurred on 2002 July 20, which is the strongest partially limb-occulted flare ever observed by the RHESSI satellite. The main results are: (1) during the main impulsive phase that lasts similar to 10 minutes, the motion of the thermal sources follows a U-shaped trajectory. Non-thermal sources move in a similar way, but in a series of larger zigzags. We further show that the non-thermal sources are actually leading the contraction motion. (2) During the main impulsive phase, X-ray sources at different energies continuously form a loop-like configuration, with the highest energy source (up to similar to 100 keV) and the lowest energy source (down to similar to 10 keV) being located at two ends. The entire loop-like configuration moves in a U-shaped trajectory, while keeping the order of descending energy from highest to lowest during motion. Two non-thermal hard Xray sources with different energies are spatially well separated in the distribution. The unusual complexities of the X-ray emissions in the tenuous solar corona challenge interpretations using bremsstrahlung in a simple magnetic configuration.

Record 35 of 247

The contracting and unshearing motion of flare loops in the X 7.1 flare on 2005 January 20 during its rising phase

Zhou, Tuan-Hui; Wang, Jun-Feng; Li, Dong; Song, Qi-Wu; Melnikov, Victor; Ji, Hai-Sheng


卷: 13; 期: 5; 页: 526-536


33

With the aim of studying the relationship between the relative motions of the loop-top (LT) source and footpoints (FPs) during the rising phase of solar flares, we give a detailed analysis of the X7.1 class flare that occurred on 2005 January 20. The flare was clearly observed by RHESSI, showing a distinct X-ray flaring loop with a bright LT source and two well-defined hard X-ray (HXR) FPs. In particular, we correct the projection effect for the positions of the FPs and magnetic polarity inversion line. We find that: (1) The LT source showed an obvious U-shaped trajectory. The source of the higher energy LT shows a faster downward/upward speed. (2) The evolution of FPs was temporally correlated with that of the LT source. The converging/separating motion of FPs corresponds to the downward/upward motion of the LT source. (3) The initial flare shear of this event is found to be nearly 50 degrees, and it has a fluctuating decrease throughout the contraction phase as well as the expansion phase. (4) Four peaks of the time profile of the unshearing rate are found to be temporally correlated with peaks in the HXR emission flux. This flare supports the overall contraction picture of flares: a descending motion of the LT source, in addition to converging and unshearing motion of FPs. All results indicate that the magnetic field was very highly sheared before the onset of the flare.

Record 36 of 247

Statistical study of UV bright points and magnetic elements from SDO observations

Li, D.; Ning, Z. J.; Wang, J. F.

NEW ASTRONOMY

卷: 23-24; 页: 19-26

We have investigated the ultraviolet bright points (UVBPs) in 14 quiet regions near the solar disk center observed by Atmospheric Imaging Assembly (AIA) onboard Solar Dynamics Observatory (SDO) from 19 to 25 in August 2010. Each region has a size of 200 x 200 arcsecs(2). In total, 2722 UVBPs at 1600 angstrom and 2963 UVBPs at 1700 angstrom are determined from the bright pixels above the mean value plus three time deviation of the background emission. Each UVBP has a minor size of 25 pixels (about 93 arcsecs(2)). The frequency distributions of these UVBPs occurrence as functions of brightness and size (area) exhibit a power-law behavior, i.e. dN/dx proportional to x-(alpha x), with an index of alpha(B) = 1.91 +/- 0.03 at 1600 angstrom and alpha(B) = 1.87 +/- 0.02 at 1700 angstrom for the

brightness, and of alpha(S) = 1.95 +/- 0.03 at 1600 angstrom and alpha(S) = 2.01 +/- 0.03 at 1700 angstrom for the size. We find that these UVBPs show a South-East direction orientation (theta) on the solar disk, whatever on the northern or southern hemispheres. We also find that the UVBPs are strongly related to the magnetic elements, which are identified from Helioseismic and Magnetic Imager (HMI) observations, indicating that the UVBPs origination from the magnetic elements. (C) 2013 Elsevier B.V. All rights reserved.

Record 37 of 247

Determination of intrinsic mode and linear mode coupling in solar microwave bursts

Huang, Guangli; Song, Qiwu; Li, Jianping

ASTROPHYSICS AND SPACE SCIENCE

卷: 345; 期: 1; 页: 41-47

An explicit equation of the propagational angle of microwave emission between the line-of-sight and the local magnetic field is newly derived based on the approximated formulae of nonthermal gyrosynchrotron emission (Dulk and Marsh in Astrophys. J. 259, 350, 1982). The existence of the solution of propagational angle is clearly shown under a series of typical parameters in solar microwave observations. It could be used to determine the intrinsic mode and linear mode coupling in solar microwave bursts by three steps. (1) The mode coupling may happen only when the angle approximately equals to 90 degrees, i.e., when the emission propagates through the quasi-transverse region (Cohen in Astrophys. J. 131, 664, 1960). (2) The inversion of polarization sense due to the weakly mode coupling takes place only when the transition frequency defined by Cohen (1960) is larger than the frequency of microwave emission, and an observable criterion of the weakly mode coupling in flaring loops was indicated by the same polarization sense in the two footpoints of a flaring loop (Melrose and Robinson in Proc. Astron. Soc. Aust. 11, 16, 1994). (3) Finally, the intrinsic mode of microwave emission is determined by the observed polarization and the calculated direction of local magnetic field according to the general plasma dispersion relation, together with the mode coupling process. However, a 180-degree ambiguity still exists in the direction of longitudinal magnetic field, to produce an uncertainty of the intrinsic mode. One example is selected to check the feasibility of the method in


34

the 2001 September 25 event with a loop-like structure nearby the central meridian passage observed by Nobeyama Radio Heliograph and Polarimeters. The calculated angle in one footpoint (FP) varied around 90(a similar to) in two time intervals of the maximum phase, which gives a direct evidence of the emission propagating through a quasi-transverse region where the linear mode coupling took place, while, the angle in another FP was always smaller than 90(a similar to) where the mode coupling did not happen. Moreover, the right-circular sense at 17 GHz was always observed in both two FPs during the event, which supports that the transition frequency should be larger than 17 GHz in the first FP together with strong magnetic field of over 2000 Gauses in photosphere, where the weakly coupled case should happen. Moreover, there are two possibilities of the intrinsic mode in the two FPs due to the 180-degree ambiguity. (1) The emission of extraordinary (X) mode from the first FP turns to the ordinary (O) mode in the two time intervals of the maximum phase, while, the X-mode is always emitted from the second FP. (2) The inversion from O-mode to X-mode takes place in the first FP, while the O-mode keeps in the second FP. If the magnetic polarities in photosphere and corona are coincident in this event, the intrinsic mode belongs to the second case.

Record 38 of 247

Frequency dependence of solar flare occurrence rates-inferred from power-law distribution

Song, Qiwu; Huang, Guangli; Huang, Yu


卷: 347; 期: 1; 页: 15-19

Based on the frequency dependence of the power-law distribution of the peak fluxes in 486 radio bursts in 1-35 GHz observed by Nobeyama Radio Polarimeters (see Song et al. in Astrophys. J. 750:160, 2012), we have first suggested in this paper that the events with power-law behaviors may be emitted from the optically-thin regions, which can be considered as a good measure for the flare energy release. This result is supported by that both the power-law and optical-thin events gradually increase with radio frequencies, which are well fitted by a power-law function with similar indices of 0.48 and 0.80, respectively. Moreover, a flare occurrence rate is newly defined by the power-law event number in per unit frequency. Its values in lower frequencies are

evidently larger than those in higher frequencies, which just imply that most flares are trigged in higher corona. Hence, the frequency variation of power-law event number may indicate different energy dissipation rates on different coronal heights.

Record 39 of 247

X-ray source motion along the loop in two solar flares

Ning, Zongjun


卷: 346; 期: 2; 页: 307-318

We explore the 3-8 keV X-ray source motion along the loop legs in two solar flares observed by the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) on August 12 and November 28, 2002. Firstly, an artificial loop is constructed to have an outline with a fixed width wide enough to cover the X-ray sources at an energy band between 3-60 keV and at various times. Secondly, RHESSI images are reconstructed at 15 energy bands with an 8 s integration window but 1 s cadence. Thirdly, the X-ray source motions are traced from the brightness distribution along the flare loop. We find that these two events tend to start as a single source at 3-8 keV around the loop top, and then separate into two which move downward along the loop legs. These two almost reach the feet of the loop at the hard X-ray (i.e. at 25-50 keV) peak. After that, the two sources move back upward to the loop top and merge together at the same position where they began. The typical timescale is about similar to 70 s, and the maximum speed can reach 1000 km s(-1). Such a downward-to-upward motion along the loop is rarely seen in the observations, and it seems to be consistent with the density evolution at the loop top, first decreasing after heating and then increasing due to evaporation.

Record 40 of 247

Chromospheric evaporation in sympathetic coronal bright points

Zhang, Q. M.; Ji, H. S.


卷: 557; 页: L5-1-L5-4

Context. Chromospheric evaporation is a key process in solar flares that has been extensively investigated using spectroscopic observations. However, direct soft X-ray (SXR) imaging of the process is rare, especially in remote brightenings associated with the primary flares that have


35

recently attracted a great deal of attention. Aims. We intend to find the evidence for chromospheric evaporation and figure out the cause of the process in sympathetic coronal bright points (CBPs), i.e., remote brightenings induced by the primary CBP. Methods. We utilised the high-cadence and high-resolution SXR observations of CBPs from the X-ray Telescope (XRT) aboard the Hinode spacecraft on 2009 August 23. Results. We discovered a thermal conduction front propagating from the primary CBP (hereafter BP1) to the first of the sympathetic CBPs (hereafter BP2) that is 60 '' away from BP1. The apparent velocity of the thermal conduction is similar to 138 km s(-1). Afterwards, hot plasma flowed upwards into the loop connecting BP1 and BP2 at a speed of similar to 76 km s(-1), a clear signature of chromospheric evaporation. Similar upflow was also observed in the loop connecting BP1 and the other sympathetic CBP (hereafter BP3) that is 80 '' away from BP1, though less significant than BP2. The apparent velocity of the upflow is similar to 47 km s (1). The thermal conduction front propagating from BP1 to BP3 was not well identified except for the jet-like motion also originating from BP1. Conclusions. We propose that the gentle chromospheric evaporation in the sympathetic CBPs were caused by thermal conduction originating from the primary CBP.

Record 41 of 247

DOUBLE POWER-LAW DISTRIBUTION OF MAGNETIC ENERGY IN THE SOLAR CORONA OVER AN ACTIVE REGION

Shen, Jinhua; Ji, Haisheng; Wiegelmann, Thomas; Inhester, Bernd


卷: 764; 期: 1; 页: 86-1-86-9

In this paper, we study the magnetic energy (ME) structure contained in the solar corona over the active region NOAA 11158. The time period is chosen as from 0: 00 to 06: 00 UT on 2011 February 15, during which an X-class flare occurred. The nonlinear force-free field (NLFFF) and the potential field extrapolation are carried out to model the coronal magnetic field over this active region, using high-quality photospheric vector magnetograms observed by the Helioseismic and Magnetic Imager on board the Solar Dynamics Observatory as boundary conditions. We find that the volume distribution for the density of the ME (B-2/8 pi) and the ohmic dissipation power (ODP, j(2)/sigma), in which j is

the electric current density (c/4 pi del x B) and sigma is the conductivity in the corona, can be readily fitted by a broken-down double-power law. The turn-over density for the spectrum of the ME and ODP is found to be fixed at similar to 1.0 x 10(4) erg cm(-3) and similar to 2.0 x 10(-15) W cm(-3) (assuming sigma = 10(5) Omega(-1) m(-1)), respectively. Compared with their first power-law spectra (fitted below the corresponding turn-over value) which remain unchanged, the second power-law spectra (fitted above the corresponding turn-over value) for the NLFFF's ME and ODP show flare-associated changes. The potential field remains steady. These results indicate that a magnetic field with energy density larger than the turn-over energy density plays a dominant role in powering the flare.

Record 42 of 247

First-Principle of the Electronic Structure and Optical Property of LaBr_3 Under High Pressure

Mao, Xiaoli; Ge, Yixian; Ma, Tao; Zhang, Jiahong

ACTA OPTICA SINICA

卷: 33; 期: 2; 页: 216002-1-216002-8

Crystal structure and electronic and optical properties of LaBr3 under high pressure are systematically investigated by first-principles method within the local-density approximation (LDA). The calculated lattice parameters and bulk modulus are in good agreement with the experimental data reported. The results of the band structure calculation show that LaBr3 is a direct-band0gap insulator without pressure, and the top of the valence band is mainly composed of Br 4p states while the lower part of the conduction band os dominated by the La 5d states…….

Record 43 of 247

Gamma-ray Spectrometer onboard Chang'E-2

Ma, T.; Chang, J.; Zhang, N.; Jian, W.; Cai, M. S.; Gong, Y. Z.; Tang, H. S.; Zhang, R. J.; Wang, N. S.; Yu, M.; Mao, J. P.; Hu, Y. M.; Xu, A. A.; Zhu, M. H.

NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS

Laboratory for Dark Matter and Space

Astronomy


36

SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT

卷: 726; 页: 113-115

Chang'E-2 gamma-ray spectrometer (GRS) is included in the payload of Chinese second lunar mission Chang'E-2 that has been launched in October 2010. Specific objectives of the GRS are to map abundance of O, Si, Fe, Ti, U, Th, K, and, perhaps, Mg, Al, and Ca, to depth of about 20 cm. The energy resolution and detection efficiency were improved compared with Chang'E-1 GRS. We will describe the design of GRS, which used LaBr3 for its main detector, and present its performance in this paper. Moreover, the initial result of Chang'E-2 GRS is reported.

Record 44 of 247

The Method to Get Background for Chang'E-1 GRS

MA, Tao; CHANG, Jin; ZHANG, Nan; WU, Jian; CAI, Mingsheng


卷: 54; 期: 4; 页: 262-369

The scientific objective of Chang’E-1 Gamma-ray spectrometer (GRS) is to study the element information including both type and abundance on the lunar surface by distinguishing the energy peak of gamma ray spectrum relative to the elements, and by calculating the peak area counts. Regretfully, the cislunar spectrum of GRS is not collected. Nevertheless, we propose a method to get the background count rate in the energy range of 0.55~2.75 MeV. The count rate map of natural

radioactive elements in 2º*2º grids is shown after reducing the background count rate. The data of Chang’s E-2 GRS is used to test the method, and the uncertainty of the result is discussed.

Record 45 of 247

Fermi/LAT observations of GRB 110625A

Tam, P.H.T.; Kong, A.K.H.; Fan, Y.-Z.

EAS Publications Series

卷: 61; 页: 83-85

We report γ-ray afterglow observations of GRB 110625A using Fermi's Large Area Telescope (LAT) above 100 MeV. Gamma-ray emission was clearly detected using data taken between 180 s and 580 s after the burst. The GeV light curve differs from a power-law decay, and probably consists of two emission periods. Simultaneous Swift/XRT

observations did not show flaring behaviors, distinguishing its origin of the extended GeV emission from the case of GRB 100728A.

Record 46 of 247

Upturn observed in heavy nuclei to iron ratios by the ATIC-2 experiment

Adams, J.H.; Ahn, H.S.; Bashindzhagyan, G.L.; Chang, J.; Christl, M.; Fazely, A.R.; Guzik, T.G.; Isbert, J.; Kim, K.C.; Kouznetsov, E.N.; Panasyuk, M.I.; Panov, A.D.; Seo, E.S.; Sokolskaya, N.V.; Watts, J.W.; Wefel, J.P.; Wu, J.; Zatsepin, V.I.

23rd European Cosmic Ray Symposium, Ecrs 2012 and 32nd Russian Cosmic Ray Conference

卷: 56; 页: 284-289

The ratios of fluxes of heavy nuclei from sulfur (Z=16) to chromium (Z=24) to the flux of iron were measured by the ATIC-2 experiment. The ratios are decreasing functions of energy from 5 GeV/n to approximately 80 GeV/n, as expected. However, an unexpected sharp upturn in the ratios are observed for energies above 100 GeV/n for all elements from Z=16 to Z=24. Similar upturn but with lower amplitude was also discovered in the ATIC-2 data for the ratio of fluxes of abundant even nuclei (C, O, Ne, Mg, Si) to the flux of iron. Therefore the spectrum of iron is significantly different from the spectra of other abundant even nuclei.

Record 47 of 247

Potassium Map from Chang ' E-2 Constraints the Impact of Crisium and Orientale Basin on the Moon

Zhu, Meng-Hua; Chang, Jin; Ma, Tao; Ip, Wing-Huen; Fa, WenZhe; Wu, Jian; Cai, MingSheng; Gong, YiZhong; Hu, YiMing; Xu, AoAo; Tang, ZeSheng

SCIENTIFIC REPORTS

卷: 3; 页: 1611-1-1611-6

KREEP materials were thought to be last crystallized at the lunar crust and mantle boundary. Impact cratering and volcanism are mainly responsible for their distributions on the lunar surface. Therefore, observation of global KREEP materials and investigation of distributions in the areas of large basins are of critical importance to understand the geologic history of the Moon. Here we report the new global potassium distribution on the Moon detected by


37

Chang'E-2 Gamma-ray Spectrometer. We found that our new measurements are in general agreement with previous observation. A new finding and an important difference is that relatively higher K abundances in the Mare Crisium and Mare Orientale than their surrounding rims were detected for the first time. In light of our observations in these two areas, we propose that Crisium and Orientale basin-forming impact events may have penetrated to the lower crust and excavate the deeper materials to the lunar surface.

Record 48 of 247

A hybrid model of GeV-TeV gamma ray emission from the Galactic center

Guo, Yi-Qing; Yuan, Qiang; Liu, Cheng; Li, Ai-Feng

JOURNAL OF PHYSICS G-NUCLEAR AND PARTICLE PHYSICS

卷: 40; 期: 6; 页: 65201-1-65201-9

The observations of high energy gamma-ray emission from the Galactic center (GC) by HESS, and recently by Fermi, suggest cosmic ray acceleration in the GC and possibly around the supermassive black hole. In this work we propose a lepton-hadron hybrid model to simultaneously explain the GeV-TeV gamma-ray emission. Both electrons and hadronic cosmic rays were accelerated during the previous activity of the GC. These particles would then diffuse outwards and interact with the interstellar gas and background radiation field. The collisions between hadronic cosmic rays with gas are responsible for the TeV gamma-ray emission detected by HESS. With fast cooling in the strong radiation field, the electrons would cool down and radiate GeV photons through inverse Compton scattering off the soft background photons. This scenario provides a natural explanation for the observed GeV-TeV spectral shape of gamma-ray.

Record 49 of 247

Theoretical study on neutron skin thickness of Ca isotopes by parity-violating electron scattering

Liu, Jian; Ren, Zhongzhou; Dong, Tiekuang

NUCLEAR PHYSICS A

卷: 900; 页: 1-15

The parity-violating electron scattering (PVS) experiment of Ca-48 has been proposed in Jefferson Lab recently. In this paper, the relation

between neutron radius of Ca-48 and corresponding parity-violating asymmetry A(pv) is investigated. With this relation, we can extract the neutron radius of Ca-48 from measurement at only one single momentum transfer. The statistical error for measuring A(pv) of Ca-48 is also calculated at the kinematics of CREx. Besides, with the study of linear dependence between Delta R-np and L, it enable us to constrain the slope L of the symmetry energy. Parity-violating electron scattering off Ca isotopes is also studied because some experimental errors can be canceled by combining PVS measurements of isotopes. To analyze the differences of neutron skin thickness of Ca isotopes, we fit the mean-field densities with 2pF distributions and study the bulk and surface contributions. By comparing the half density radius and surface parameter along Ca isotopes, we note there may exist neutron halo nuclei in the extreme neutron rich range.

Record 50 of 247

constraints on the dark matter annihilation scenario of Fermi 130 GeV gamma-ray line emission by continuous gamma-rays, Milky Way halo, galaxy clusters and dwarf galaxies observations

Huang, Xiaoyuan; Yuan, Qiang; Yin, Peng-Fei; Bi, Xiao-Jun; Chen, Xuelei


期: 5; 页: E02-1

It was recently reported that there may exist monochromatic $\gamma$-ray emission at $\sim 130$ GeV from the Galactic center in the Fermi Large Area Telescope data, which might be related with dark matter (DM) annihilation. In this work we carry out a comprehensive check of consistency of the results with the DM annihilation scenario, using the 3.7 yrs Fermi observation of the inner Galaxy, Galactic halo, clusters of galaxies and dwarf galaxies. The results found are as follows. 1) Very strong constraints on the DM annihilation into continuous $\gamma$-rays from the Galactic center are set, which are as stringent as the "natural" scale assuming thermal freeze-out of DM. Such limit sets strong constraint on the DM models to explain the line emission. 2) No line emission from the Galactic halo is found in the Fermi data, and the constraints on line emission is marginally consistent with the DM annihilation interpretation


38

of the $\sim 130$ GeV line emission from the inner Galaxy. 3) No line emission from galaxy clusters and dwarf galaxies is detected, although possible concentration of photons from clusters in 120-140 GeV is revealed. The constraints from clusters and dwarf galaxies are weak and consistent with the DM annihilation scenario to explain the $\sim 130$ GeV line emission.

Record 51 of 247

A generic method to constrain the dark matter model parameters from Fermi observations of dwarf spheroids

Tsai, Yue-Lin Sming; Yuan, Qiang; Huang, Xiaoyuan


期: 3; 页: 18-1-18-14

Observation of gamma-rays from dwarf galaxies is an effective way to search for particle dark matter. Using 4-year data of Fermi-LAT observations on a series of Milky Way satellites, we develop a general way to search for the signals from dark matter annihilation in such objects. Instead of giving prior information about the energy spectrum of dark matter annihilation, we bin the Fermi-LAT data into several energy bins and build a likelihood map in the "energy bin - flux" plane. The final likelihood of any spectrum can be easily derived through combining the likelihood of all the energy bins. It gives consistent result with that directly calculated using the Fermi Scientific Tool. This method is very efficient for the study of any specific dark matter models with gamma-rays. We use the new likelihood map with Fermi-LAT 4 year data to fit the parameter space in three representative dark matter models: i) toy dark matter model, ii) effective dark matter operators, and iii) supersymmetric neutralino dark matter.

Record 52 of 247

Dissecting X-ray-Emitting Gas Around the Center of Our Galaxy

Wang, Q. D.; Nowak, M. A.; Markoff, S. B.; Baganoff, F. K.; Nayakshin, S.; Yuan, F.; Cuadra, J.; Davis, J.; Dexter, J.; Fabian, A. C.; Grosso, N.; Haggard, D.; Houck, J.; Ji, L.; Li, Z.; Neilsen, J.; Porquet, D.; Ripple, F.; Shcherbakov, R. V.

SCIENCE

卷: 341; 期: 6149; 页: 981-983

Most supermassive black holes (SMBHs) are

accreting at very low levels and are difficult to distinguish from the galaxy centers where they reside. Our own Galaxy's SMBH provides an instructive exception, and we present a close-up view of its quiescent x-ray emission based on 3 megaseconds of Chandra observations. Although the x-ray emission is elongated and aligns well with a surrounding disk of massive stars, we can rule out a concentration of low-mass coronally active stars as the origin of the emission on the basis of the lack of predicted iron (Fe) K alpha emission. The extremely weak hydrogen (H)-like Fe K alpha line further suggests the presence of an outflow from the accretion flow onto the SMBH. These results provide important constraints for models of the prevalent radiatively inefficient accretion state.

Record 53 of 247

Nuclear charge radii of heavy and superheavy nuclei from the experimental alpha-decay energies and half-lives

Ni, Dongdong; Ren, Zhongzhou; Dong, Tiekuang; Qian, Yibin

PHYSICAL REVIEW C

卷: 87; 期: 2; 页: 24310-1-24310-9

The radius of a nucleus is one of the important quantities in nuclear physics. Although there are many researches on ground-state properties of superheavy nuclei, researches on charge radii of superheavy nuclei are rare. In this article, nuclear root-mean-square (rms) charge radii of heavy and superheavy nuclei are extracted from the experimental alpha-decay data. alpha-decay calculations are performed within the generalized density-dependent cluster model, where alpha-decay half-lives are evaluated using quasibound state wave functions. The charge distribution of daughter nuclei is determined in the double-folding model to reproduce the experimental alpha-decay half-lives. The rms charge radius is then calculated using the resulting charge distribution. In addition, a simple formula is also proposed to calculate nuclear charge radii with the experimental alpha-decay energies and half-lives. The formula is directly derived from the Wentzel-Kramers-Brillouin barrier penetration probability with some approximations. The two different methods show good agreement with the experimental data for even-even nuclei, and the deduced results are consistent with other theoretical models. Moreover, nuclear radii of


39

heavy and superheavy nuclei with Z = 98-116 are extracted from the alpha-decay data, for which alpha decay is a unique tool to probe nuclear sizes at present. This is the first result on nuclear charge radii of superheavy nuclei based on the experimental alpha-decay data.

Record 54 of 247

THE NARROW X-RAY TAIL AND DOUBLE H alpha TAILS OF ESO 137-002 IN A3627

Zhang, B.; Sun, M.; Ji, L.; Sarazin, C.; Lin, X. B.; Nulsen, P. E. J.; Roediger, E.; Donahue, M.; Forman, W.; Jones, C.; Voit, G. M.; Kong, X.


卷: 777; 期: 2; 页: 122-1-122-13

We present the analysis of a deep Chandra observation of a similar to 2L(*) late-type galaxy, ESO 137-002, in the closest rich cluster A3627. The Chandra data reveal a long (greater than or similar to 40 kpc) and narrow tail with a nearly constant width (similar to 3 kpc) to the southeast of the galaxy, and a leading edge similar to 1.5 kpc from the galaxy center on the upstream side of the tail. The tail is most likely caused by the nearly edge-on stripping of ESO 137-002's interstellar medium (ISM) by ram pressure, compared to the nearly face-on stripping of ESO 137-001 discussed in our previous work. Spectral analysis of individual regions along the tail shows that the gas throughout it has a rather constant temperature, similar to 1 keV, very close to the temperature of the tails of ESO 137-001, if the same atomic database is used. The derived gas abundance is low (similar to 0.2 solar with the single-kT model), an indication of the multiphase nature of the gas in the tail. The mass of the X-ray tail is only a small fraction (<5%) of the initial ISM mass of the galaxy, suggesting that the stripping is most likely at an early stage. However, with any of the single-kT, double-kT, and multi-kT models we tried, the tail is always "over-pressured" relative to the surrounding intracluster medium (ICM), which could be due to the uncertainties in the abundance, thermal versus non-thermal X-ray emission, or magnetic support in the ICM. The H alpha data from the Southern Observatory for Astrophysical Research show a similar to 21 kpc tail spatially coincident with the X-ray tail, as well as a secondary tail (similar to 12 kpc long) to the east of the main tail diverging at an angle of similar to 23 degrees and starting at a distance of similar to 7.5 kpc from the nucleus. At the position

of the secondary H alpha tail, the X-ray emission is also enhanced at the similar to 2 sigma level. We compare the tails of ESO 137-001 and ESO 137-002, and also compare the tails to simulations. Both the similarities and differences of the tails pose challenges to the simulations. Several implications are briefly discussed.

Record 55 of 247

Gamma-ray Spectrometer onboard Chang'E-2

Ma, T.; Chang, J.; Zhang, N.; Cai, M. S.; Gong, Y. Z.; Tang, H. S.; Zhang, R. J.; Wang, N. S.; Yu, M.; Hu, Y. M.


卷: 54; 期: 3; 页: 291-299

The Chang’E-2 Gamma-Ray Spectrometer (GRS) is included in the payload of Chinese second lunar mission Chang’E-2, which has been launched in Oct, 2010. Specific objectives of the GRS are to map the abundance of O, Si, Fe, Ti, U, Th, K, and perhaps, Mg, Al, and Ca, to the depths of about 20 cm. The energy resolution and detecting efficiency are improved in comparison with the Chang’E-1 GRS. We describe the design of the GRS and present its performance in this paper. Moreover, the initial results of Chang’E-2 GRS are reported.

Record 56 of 247

PAMELA/Fermi-LAT electron cosmic ray spectrum at similar to 100 GeV: Implication for dark matter annihilation signal in accordance with the 130 GeV gamma-ray line

Feng, Lei; Yuan, Qiang; Li, Xiang; Fan, Yi-Zhong

PHYSICS LETTERS B

卷: 720; 页: 39450-1-39450-5

Recently, a tentative 130 GeV gamma-ray line signal was identified by quite a few groups. If correct it would constitute a "smoking gun" for dark matter annihilations. Interestingly, the spectra of the cosmic ray electrons detected by PAMELA and Fermi-LAT. both show tiny wiggle-like structure at similar to 100 GeV, which might indicate a weak signal of the annihilation of similar to 130 GeV dark matter particles into electrons/positrons with a velocity-weighted cross section (sigma nu)chi chi -> e(+),e(-) similar to 4 x 10(-26) cm(3) s(-1). The prospect of identifying such a potential weak dark-matter-annihilation electron and/or positron component by AMS-02, a mission.to measure the high energy cosmic ray


40

spectra with unprecedented accuracy, is investigated.

Record 57 of 247

Diffuse PeV neutrino emission from ultraluminous infrared galaxies

He, Hao-Ning; Wang, Tao; Fan, Yi-Zhong; Liu, Si-Ming; Wei, Da-Ming

PHYSICAL REVIEW D

卷: 87; 期: 6; 页: 63011-1-63011-5

Ultraluminous infrared galaxies (ULIRGs) are the most luminous and intense starburst galaxies in the Universe. Both their star formation rates and their gas surface mass densities are very high, implying a high supernova rate and an efficient energy conversion of energetic protons. A small fraction of these supernovae are the so-called hypernovae, with a typical kinetic energy similar to 10(52) erg and a shock velocity >= 10(9) cm s(-1). The strong shocks driven by hypernovae are able to accelerate cosmic ray protons up to 1017 eV. These energetic protons lose a good fraction of their energy through proton-proton collision when ejected into very dense interstellar media, and as a result, produce high-energy neutrinos (<= 5 PeV). Recent deep infrared surveys provide solid constraints on the number density of ULIRGs across a wide redshift range 0 <= z <= 2.3, allowing us to derive the flux of diffuse neutrinos from hypernovae. We find that at PeV energies, the diffuse neutrinos contributed by ULIRGs are comparable to atmosphere neutrinos with the flux of 2 x 10(-9) GeV cm(-2) s(-1) sr(-1) by assuming the injected cosmic ray spectrum to be dN(p)'/d epsilon(p)' proportional to epsilon(p)'(-2).

Record 58 of 247

Signature of gravitational wave radiation in afterglows of short gamma-ray bursts?

Fan, Yi-Zhong; Wu, Xue-Feng; Wei, Da-Ming

PHYSICAL REVIEW D

卷: 88; 期: 6; 页: 67304-1-67304-4

Short gamma-ray bursts (GRBs), brief intense emission of gamma rays characterized by a duration shorter than 2 s that are plausibly powered by the coalescence of binary neutron stars, are believed to be strong gravitational wave radiation (GWR) sources. The test of such a speculation has been thought to be impossible until the performance of the detectors like

advanced LIGO. Recently there has been growing evidence for the formation of a highly magnetized neutron star (i.e., magnetar) in the double neutron star mergers. In this work we reexamine the interpretation of the x-ray plateau followed by an abrupt decline detected in some short GRB afterglows within the supramassive magnetar model and find that the maximum gravitational mass of the nonrotating neutron stars is similar to 2.3M(circle dot) and the observed duration of some x-ray plateaus are significantly shorter than that expected in the magnetic dipole radiation scenario, suggesting that the collapse of the supramassive magnetars has been considerably enhanced by the energy loss via GWR. Such a result demonstrates that the signature of GWR may have already existed in current electromagnetic data of short GRBs.

Record 59 of 247

Decaying asymmetric dark matter relaxes the AMS-Fermi tension

Feng, Lei; Kang, Zhaofeng


期: 10; 页: 8-1-8-15

The first result of AMS-02 confirms the positron fraction excess observed by PAMELA, but the spectrum is somewhat softer than that of PAMELA. In the dark matter (DM) interpretation it brings a tension between AMS-02 and Fermi-LAT, which reported an excess of the electron plus positron flux. In this work we point out that the asymmetric cosmic ray from asymmetric dark matter (ADM) decay relaxes the tension. It is found that in the case of two-body decay a bosonic ADM around 2.4 TeV and decaying into mu(-)tau(+) can significantly improve the fits. Based on the R-parity-violating supersymmetry with operators LLEe, we propose a minimal model to realize that ADM. The model introduces only a pair of singlets (X, (X) over bar) with a tiny coupling LHuX, which makes the ADM share the lepton asymmetry and decay into mu(-)tau(+) along the operator LLEe.

Record 60 of 247

A Supramassive Magnetar Central Engine for GRB 130603B

Fan, Yi-Zhong; Yu, Yun-Wei; Xu, Dong; Jin, Zhi-Ping; Wu, Xue-Feng; Wei, Da-Ming; Zhang, Bing


41


卷: 779; 期: 2; 页: L25-1-L25-4

We show that the peculiar early optical emission and, in particular, the X-ray after glow emission of the short-duration burst GRB 130603B can be explained by continuous energy injection into the blastwave from a supramassive magnetar central engine. The observed energetics and temporal/spectral properties of the late infrared bump (i.e., the "kilonova") are also found to be consistent with emission from the ejecta launched during a neutron star (NS)-NS merger and powered by a magnetar central engine. The isotropic-equivalent kinetic energies of both the gamma-ray burst (GRB) blastwave and the kilonova are approximately E-k similar to 10(51) erg, consistent with being powered by a near-isotropic magnetar wind. However, this relatively small value requires that most of the initial rotational energy of the magnetar (similar to a few x 10(52) erg) is carried away by gravitational wave radiation. Our results suggest that (1) the progenitor of GRB 130603B was a NS-NS binary system, the merger product of which would have been a supramassive NS that lasted for about similar to 1000 s; (2) the equation of state of the nuclear matter should be stiff enough to allow the survival of a long-lived supramassive NS; thus this suggested that the detection of the bright electromagnetic counterparts of gravitational wave triggers without short GRB associations is promising in the upcoming Advanced LIGO/VIRGO era.

Record 61 of 247

HIGH-ENERGY EMISSION OF GRB 130427A: EVIDENCE FOR INVERSE COMPTON RADIATION

Fan, Yi-Zhong; Tam, P. H. T.; Zhang, Fu-Wen; Liang, Yun-Feng; He, Hao-Ning; Zhou, Bei; Yang, Rui-Zhi; Jin, Zhi-Ping; Wei, Da-Ming


卷: 776; 期: 2; 页: 95-1-95-9

A nearby superluminous burst GRB 130427A was simultaneously detected by six gamma-ray space telescopes (Swift, the Fermi GLAST Burst Monitor (GBM)/Large Area Telescope, Konus-Wind, SPI-ACS/INTEGRAL, AGILE, and RHESSI) and by three RAPTOR full-sky persistent monitors. The isotropic gamma-ray energy release is similar to 10(54) erg, rendering it the most powerful explosion among gamma-ray bursts (GRBs) with a redshift z <= 0.5. The emission above 100 MeV

lasted about one day, and four photons are at energies greater than 40 GeV. We show that the count rate of 100 MeV-100 GeV emission may be mainly accounted for by the forward shock synchrotron radiation and the inverse Compton radiation likely dominates at GeV-TeV energies. In particular, an inverse Compton radiation origin is favored for the similar to(95.3, 47.3, 41.4, 38.5, 32) GeV photons arriving at t similar to (243, 256.3, 610.6, 3409.8, 34366.2) s after the trigger of Fermi-GBM. Interestingly, the external inverse Compton scattering of the prompt emission (the second episode, i.e., t similar to 120-260 s) by the forward-shock-accelerated electrons is expected to produce a few gamma-rays at energies above 10 GeV, while five were detected in the same time interval. A possible unified model for the prompt soft gamma-ray, optical, and GeV emission of GRB 130427A, GRB 080319B, and GRB 090902B is outlined. Implications of the null detection of >1 TeV neutrinos from GRB 130427A by IceCube are discussed.

Record 62 of 247

CONSTRAINING THE DISTRIBUTION OF DARK MATTER IN THE INNER GALAXY WITH AN INDIRECT DETECTION SIGNAL: THE CASE OF A TENTATIVE 130 GeV gamma-RAY LINE

Yang, Rui-Zhi; Feng, Lei; Li, Xiang; Fan, Yi-Zhong


卷: 770; 期: 2; 页: 127-1-127-5

Dark matter distribution in the very inner region of our Galaxy is still debated. In N-body simulations, a cuspy dark matter halo density profile is favored. Several dissipative baryonic processes, however, are found to be able to significantly flatten dark matter distribution, and a cored dark matter halo density profile is possible. Baryons dominate the gravitational potential in the inner Galaxy, hence a direct constraint on the abundance of dark matter particles is rather challenging. Recently, a few groups have identified a tentative 130 GeV line signal in the Galactic center, which could be interpreted as the signal of dark matter annihilation. Using current 130 GeV line data and adopting the generalized Navarro-Frenk-White profile of the dark matter halo-local dark matter density rho(0) = 0.4 GeV cm(-3) and r(s) = 20 kpc-we obtain a 95% confidence level lower (upper) limit on the inner slope of dark matter density distribution, alpha = 1.06 (the cross section of dark matter annihilation


42

into gamma-rays <sigma nu > (xx -> gamma gamma) = 1.3 x 10(-27) cm(3) s(-1)). Such a slope is consistent with the results of some N-body simulations and, if the signal is due to dark matter, suggests that baryonic processes may be unimportant.

Record 63 of 247

Reconcile the AMS-02 positron fraction and Fermi-LAT/HESS total e(+/-) spectra by the primary electron spectrum hardening

Yuan, Qiang ;Bi, Xiao-Jun

PHYSICS LETTERS B

卷:727;期:1-3;页:1-7

The recently reported positron fraction up to similar to 350 GeV by AMS-02 seems to have tension with the total electron/positron spectra detected by Fermi and HESS, for either pulsar or dark matter annihilation/decay scenario as the primary positron sources. In this work we will show that the tension will be removed by an adjustment of the primary electron spectrum. If the primary electron spectrum becomes harder above similar to 50 GeV, similar as the cosmic ray nuclei spectrum, the AMS-02 positron fraction and Fermi/HESS data can be well fitted by both the pulsar and dark matter models. This result may be suggestive of a common origin of the cosmic ray nuclei and the primary electrons. Furthermore, this study also implies that the properties of the extra sources derived from the fitting to the AMS-02 data should depend on the form of background. (C) 2013 Elsevier B.V. All rights reserved.

Record 64 of 247

Evidence For A Second Component In The High-Energy Core Emission From Centaurus A?

Sahakyan, N. ; Yang, R. ; Aharonian, F. A. ;Rieger, F. M.


卷:770;期:1;页: L6(1-5)

We report on an analysis of Fermi Large Area Telescope data from four years of observations of the nearby radio galaxy Centaurus A (Cen A). The increased photon statistics results in a detection of high-energy (>100 MeV) gamma-rays up to 50 GeV from the core of Cen A, with a detection significance of about 44 sigma. The average gamma-ray spectrum of the core reveals evidence for a possible deviation from a simple power law. A likelihood analysis with a broken power-law model shows that the photon index becomes harder above E-b similar or equal to 4 GeV, changing from Gamma(1) = 2.74 +/- 0.03 below to Gamma(2) = 2.09 +/- 0.20 above. This hardening could be caused by the contribution of an additional high-energy component beyond the common synchrotron self-Compton jet emission. No clear evidence for variability in the high-energy domain is seen. We compare our results with the spectrum reported by H.E.S.S. in the TeV energy range and discuss possible origins of the hardening observed.


43

II. Antarctic Astronomy Radio Astronomy

Record 65 of 247

Notes on the CCD Flatfields of the YFOSC on the 2.4m Reflector of the Yunnan Observatory

YAO, Baoan; ZHANG, Chunsheng

ASTRONOMICAL RESEARCH AND TECHNOLOGY

卷: 10; 期: 3; 页: 283-287

Similar to the BFOSC mounted on the 2.16m reflector of the National Observatories at the Xinglong station, the YFOSC instrument is mounted on the 2.4m reflector of the Yunnan Observatory. We measured the CCD flatfields of the YFOSC in the direct imaging mode in the V band. We constructed an average flatfield for the flatfields observed at different CCD orientation angles. It has the maximum error of 0.015mag. Unlike the direct-imaging VersArray CCD camera at the Cassegrain focus, the maximum error for the YFOSC cannot be less than 0.005mag even within the 6.'5-diameter central circular region of its field of view. The causes for the difference are as follows. The errors for the VersArray CCD are only due to the uncorrected scattered light from the baffles of the 2.4m reflector, but those for the YFOSC are further contributed by the uncorrected scattered light inside the YFOSC itself. We expect that errors for the B-, R-, and I-band flatfields are similar since the same error sources are present. Fringes will appear in R-and I-band images obtained with the YFOSC. This is due to the interference of the night-sky emission lines within the silicon of the CCD. A V-band image does not suffer from this effect because shorter-wavelength emission lines are absorbed more by the silicon, and are weaker and fewer. The fringing is an additive effect. The fringing patterns must be subtracted from CCD images.

Record 66 of 247

A Theoretical Probe for Excitation Mechanism of Solar-like and Mira-like Oscillations of Stars

Xiong Darun; Deng Licai

Acta Astronomica Sinica

卷: 54; 期: 1; 页: 20-25

The linear stability analysis of the radial and non-radial oscillations for the evolutionary models

of the star with a mass of 0.6~3M⊙ is takec by using a nonlocal and time-dependent convection theory. The results show that the unstable low-temperature stars on the right side of instability strip can be divided into two groups……

Record 67 of 247

Seismic study of solar convection and overshooting: results of nonlocal convection

Zhang, Chun-Guang; Deng, Li-Cai; Xiong, Da-Run; Christensen-Dalsgaard, Jorgen


卷: 13; 期: 9; 页: 1127-1140

Local mixing-length theory is incapable of describing nonlocal phenomena in stellar convection, such as overshooting. Therefore standard solar models constructed with local mixing-length theory significantly deviate from the Sun at the boundaries of the convection zone, where convection becomes less efficient and nonlocal effects are important. The differences between observed and computed frequencies mainly come from the region near the surface, while the localized difference in sound speed is just below the convective envelope. We compute a solar envelope model using Xiong's nonlocal convection theory, and carry out helioseismic analysis. The nonlocal model has a smooth transition at the base of the convection zone, as revealed by helioseismology. It reproduces solar frequencies more accurately, and reduces the localized difference in sound speed between the Sun and standard solar models.

Record 68 of 247

Solar-like and Mira-like oscillations of stars - A uniform excitation mechanism

Xiong, Da-Run; Deng, Li-Cai


卷: 13; 期: 11; 页: 1269-1294

Using a non-local and time-dependent theory of

Stellar Structure, Evolution and Pulsation


44

convection, we have calculated the linear non-adiabatic oscillations of the radial and low-degree F-p39 modes for evolutionary models from the main sequence to the asymptotic giant branch for stars with solar abundance (X = 0. 7 0, Z = 0. 0 2) in the mass range of 0.6-3.0 M circle dot. The results show that low luminosity cool stars tend to be solar-like oscillators, whose low-order modes are stable, but intermediate and high order p-modes are pulsationally unstable; their unstable modes have a wide range in frequency and small values for amplitude growth rates. For stars with increasing luminosity and therefore lower temperature, the unstable modes shift towards lower orders, the corresponding range of frequency decreases, and the amplitude growth rate increases. High luminosity red giant stars behave like typical Mira-like oscillators. The effects of the coupling between convection and oscillations on pulsational instability have been carefully analyzed in this work. Our research shows that convection does not simply act as a damping mechanism for oscillations, and the complex nature of the coupling between convection and oscillations makes turbulent convection sometimes behave as damping, and sometimes as excitation. Such a picture can not only naturally account for the red edge of the instability strip, but also the solar-like oscillations in low luminosity red stars and Mira-like ones in high luminosity red giants.

Record 69of 247

Are there Pulsationally Unstable Low-degree p1 Modes in the Sun

Xiong Da-run; Deng Li-cai


卷: 37; 期: 3; 页: 294-301

By using a non-local time-dependent theory of stellar convection, the solar non-adiabatic pulsations of the low- and intermediate-degree (l< 25) modes are calculated. The results show that the non-radial p1 modes of l = 1-5 are pulsationally unstable. However, the adjacent g, f, p2-p5 modes and the p1 modes of l > 5 are stable. From the analysis of the diagram of integrated work it is discovered that the excitation of oscillations comes from the radiation zone beneath the convective region. Whether the sun possesses unstable low-degree p1 modes is of significant importance for clarifying the excitation mechanism of solar five-minute oscillations.

Record 70 of 247

A theoretical Probe for Excitation Mechanisms of Sun-like and Mira-like Oscillations of Stars

Xiong Da-run; Deng Li-cai


卷: 37; 期: 1; 页: 1-7

The linear nonadiabatic oscillations for evolutionary models of 0.6- 3M8 stars are calculated by using a nonlocal and time-dependent convection theory. The results show that in the HR diagram the pulsation-unstable low- temperature stars on the right side of instability strip can be divided into two groups. One group indicates the Sun-like oscillation stars composed of the main- sequence dwarfs, sub-giants and red giants (RGs) of low and intermediate luminosities, which are unstable in

the intermediate- and high-order (n ≥ 12) p-

modes, and stable in the low-order (n ≤ 5) p-modes. Another group indicates the Mira-like stars composed of the bright RGs and asymptotic giant branch (AGB) stars, which are just contrary

to Sun-like stars, unstable in low-order (n≤5) p-modes and stable in the intermediate- and

high-order (n≥12) p-modes. The oscillations for

the red edge of Cepheid (δ Scuti) instability strip, Sun-like and Mira-like stars can be explained uniformly by the coupling between convection and oscillation (CCO). For the low-temperature stars on the right side of instability strip, CCO is the dominant excitation and damping mechanism of the oscillations of low- and intermediate-order p-modes, and the turbulent stochastic excitation becomes important only for the high-order p-modes of Sun-like oscillations.

Record71of 247

The simulation techniques and applications in modern cosmology

Feng, LongLong; Zhu, Weishan

SCIENCE SINICA Physica, Mechanica & Astronomica

卷: 43; 期: 6; 页: 687-707

The diversity and highly nonlinearity in physical processes occurred on comic scales has made the simulation technique an essential and powerful

Center for Antarctic Astronomy


45

tool of modern cosmology researches. It can not only be applied to track the formation and evolution of the cosmic structures, and also bridges the gap between the astronomical observations and theoretical models. This articles is going to give a short review of state of the art of computational cosmology, including the N-body simulation techniques for collisionless particles and computational hydrodynamics with baryonic physics. Moreover, we will target the core scientific questions in modern cosmology, and present a brief summary of applications of extremely large simulations in next generation sky survey especially designed for detections of dark matter and dark energy. In addition, we describe a few highlights of numerical simulation in studying the formation of the first stars, the first galaxies, cold gas accretions and star formation as well as galactic disk formation at high redshifts. In accordance to the upcoming large sky surveys and the rapid progresses made in supercomputing technology, we give an outlook for the next decade, a perspective of what computational challenges will be met, and what exciting headway can be expected in computational cosmology and relative sciences.

Record 72 of 247

Turbulence effect of the intergalactic medium

Zhu, Weishan


卷: 54; 期: 4; 页: 401-402

The turbulence in the intergalactic medium (IGM) and its impact on the clustering of baryonic matter are investigated with the cosmological

hydrodynamic simulation in the Λ CDM framework the observational tools that may be used to verify the possibility of the turbulence in the IGM are also discussed.

Record 73 of 247

Gravitational lensing effects on submillimetre galaxy counts

Er, Xinzhong; Li, Guoliang; Mao, Shude; Cao, Liang


卷: 430; 期: 2; 页: 1423-1432

We study the effects on the number counts of submillimetre galaxies due to gravitational lensing. We explore the effects on the magnification

cross-section due to halo density profiles, ellipticity and cosmological parameter (the power-spectrum normalization sigma(8)). We show that the ellipticity does not strongly affect the magnification cross-section in gravitational lensing while the halo radial profiles do. Since the baryonic cooling effect is stronger in galaxies than clusters, galactic haloes are more concentrated. In light of this, a new scenario of two-halo-population model is explored where galaxies are modelled as a singular isothermal sphere profile and clusters as a Navarro, Frenk and White profile. We find that the transition mass between the two has modest effects on the lensing probability. The cosmological parameter sigma(8) alters the abundance of haloes and therefore affects our results. Compared with other methods, our model is simpler and more realistic. The conclusions of previous works confirm that gravitational lensing is a natural explanation for the number count excess at the bright end.

Record 74 of 247

The mass profile and accretion history of cold dark matter haloes

Ludlow, Aaron D.; Navarro, Julio F.; Boylan-Kolchin, Michael; Bett, Philip E.; Angulo, Raul E.; Li, Ming; White, Simon D. M.; Frenk, Carlos; Springel, Volker


卷: 432; 期: 2; 页: 1103-1113

We use the Millennium Simulation series to investigate the relation between the accretion history and mass profile of cold dark matter (CDM) haloes. We find that the mean inner density within the scale radius, r(-2) (where the halo density profile has isothermal slope), is directly proportional to the critical density of the Universe at the time when the virial mass of the main progenitor equals the mass enclosed within r(-2). Scaled to these characteristic values of mass and density, the average mass accretion history, expressed in terms of the critical density of the Universe, M((crit)(z)), resembles that of the enclosed density profile, M(<<>>), at z = 0. Both follow closely the Navarro, Frenk & White (NFW) profile, which suggests that the similarity of halo mass profiles originates from the mass-independence of halo accretion histories. Support for this interpretation is provided by outlier haloes whose accretion histories deviate


46

from the NFW shape; their mass profiles show correlated deviations from NFW and are better approximated by Einasto profiles. Fitting both M(<<>>) and M((crit)) with either NFW or Einasto profiles yield concentration and shape parameters that are correlated, confirming and extending earlier work that has linked the concentration of a halo with its accretion history. These correlations also confirm that halo structure is insensitive to initial conditions: only haloes whose accretion histories differ greatly from the NFW shape show notable deviations from NFW in their mass profiles. As a result, the NFW profile provides acceptable fits to hot dark matter haloes, which do not form hierarchically, and for fluctuation power spectra other than CDM. Our findings, however, predict a subtle but systematic dependence of mass profile shape on accretion history which, if confirmed, would provide strong support for the link between accretion history and halo structure we propose here.

Record 75 of 247

A Complete Reference of the Analytical Synchrotron External Shock Models of Gamma-Ray Bursts

Gao, He; Lei, Wei-Hua; Zou, Yuan-Chuan; Wu, Xue-Feng; Zhang, Bing

New Astronomy Reviews

卷: 57; 期: 5; 页: 141-190

Gamma-ray bursts are most luminous explosions in the universe. Their ejecta are believed to move towards Earth with a relativistic speed. The

interaction between this “relativistic jet” and a circumburst medium drives a pair of (forward and reverse) shocks. The electrons accelerated in these shocks radiate synchrotron emission to power the broad-band afterglow of GRBs. The external shock theory is an elegant theory, since it invokes a limit number of model parameters, and has well predicted spectral and temporal properties. On the other hand, depending on many factors (e.g. the energy content, ambient density profile, collimation of the ejecta, forward vs. reverse shock dynamics, and synchrotron spectral regimes), there is a wide variety of the models. These models have distinct predictions on the afterglow decaying indices, the spectral indices, and the relations between them (the

so-called “closure relations”), which have been widely used to interpret the rich multi-wavelength afterglow observations. This review article

provides a complete reference of all the analytical synchrotron external shock afterglow models by deriving the temporal and spectral indices of all the models in all spectral regimes, including some regimes that have not been published before. The review article is designated to serve as a useful tool for afterglow observers to quickly identify relevant models to interpret their data. The limitations of the analytical models are reviewed, with a list of situations summarized when numerical treatments are needed.

Record 76 of 247

Peculiar velocity decomposition, redshift space distortion, and velocity reconstruction in redshift surveys: The methodology

Zhang, Pengjie; Pan, Jun; Zheng, Yi

PHYSICAL REVIEW D

卷: 87; 期: 6; 页: 063526-1-063526-17

Massive spectroscopic surveys will measure the redshift space distortion (RSD) induced by galaxy peculiar velocity to unprecedented accuracy and open a new era of precision RSD cosmology. We develop a new method to improve the RSD modeling and to carry out robust reconstruction of the 3D large scale peculiar velocity through galaxy redshift surveys, in light of RSD. (1) We propose a mathematically unique and physically motivated decomposition of peculiar velocity into three eigencomponents: an irrotational component completely correlated with the underlying density field (v(delta)), an irrotational component uncorrelated with the density field (v(S)), and a rotational (curl) component (v(B)). The three components have different origins, different scale dependences, and different impacts on RSD. (2) This decomposition has the potential to simplify and improve the RSD modeling. (i) v(B) damps the redshift space clustering. (ii) v(S) causes both damping and enhancement to the redshift space power spectrum P-s(k, u). Nevertheless, the leading order contribution to the enhancement has a u(4) directional dependence, distinctively different from the Kaiser formula. Here, u equivalent to k(z)/k, k is the amplitude of the wave vector, and k(z) is the component along the line of sight. (iii) v(delta) is of the greatest importance for the RSD cosmology. We find that the induced redshift clustering shows a number of important deviations from the usual Kaiser formula. Even in the limit of v(S) -> 0 and v(B) -> 0, the leading


47

order contribution alpha (1 + f (W) over tilde (k)u(2))(2) . It differs from the Kaiser formula by a window function (W) over tilde (k).Nonlinear evolution generically drives (W) over tilde (k) <= 1. We hence identify a significant systematical error causing underestimation of the structure growth parameter f by as much as O(10%) even at a relatively large scale k = 0.1h/Mpc. (iv) The velocity decomposition reveals the three origins of the "finger-of-God'' (FOG) effect and suggests how to simplify and improve the modeling of FOG by treating the three components separately. (v) We derive a new formula for the redshift space power spectrum. Under the velocity decomposition scheme, all high order Gaussian corrections and non-Gaussian corrections of order delta(3) can be taken into account without introducing extra model uncertainties. Here delta is the nonlinear overdensity. (3) The velocity decomposition clarifies issues in peculiar velocity reconstruction through 3D galaxy distribution. We discuss two possible ways to carry out the 3D v(delta) reconstruction. Both use the otherwise troublesome RSD in velocity reconstruction as a valuable source of information. Both have the advantage of rendering the reconstruction of a stochastic 3D field into the reconstruction of a deterministic window function W-s(k,u) of limited degrees of freedom. Both can automatically and significantly alleviate the galaxy bias problem and, in the limit of a deterministic galaxy bias, completely overcome it. Part 1 of this series of works lays out the methodology. Companion papers Y. Zheng et al. (in preparation). will extensively evaluate its performance against N-body simulations.

Record 77 of 247

Compton scattering of self-absorbed synchrotron emission

Gao, He; Lei, Wei-Hua; Wu, Xue-Feng; Zhang, Bing


卷: 435; 期: 3; 页: 2520-2531

Synchrotron self-Compton (SSC) scattering is an important emission mechanism in many astronomical sources, such as gamma-ray bursts (GRBs) and active galactic nuclei. We give a complete presentation of the analytical approximations for the Compton scattering of synchrotron emission with both weak and strong synchrotron self-absorption. All possible orders of

the characteristic synchrotron spectral breaks (nu(a), nu(m) and nu(c)) are studied. In the weak self-absorption regime, i.e. nu(a) < nu(c), the electron energy distribution is not modified by the self-absorption process. The shape of the SSC component broadly resembles that of synchrotron, but with the following features: The SSC flux increases linearly with frequency up to the SSC break frequency corresponding to the self-absorption frequency nu(a); and the presence of a logarithmic term in the high-frequency range of the SSC spectra makes it harder than the power-law approximation. In the strong absorption regime, i.e. nu(a) > nu(c), heating of low-energy electrons due to synchrotron absorption leads to pile-up of electrons, and form a thermal component besides the broken power-law component. This leads to two-component (thermal + non-thermal) spectra for both the synchrotron and SSC spectral components. For nu(c) < nu(a) < nu(m), the spectrum is thermal (non-thermal) dominated if nu(a) > root nu(m)nu(c) (nu(a) < root nu(m)nu(c)). Similar to the weak-absorption regime, the SSC spectral component is broader than the simple broken power-law approximation. We derive the critical condition for strong absorption (electron pile-up), and discuss a case of GRB reverse shock emission in a wind medium, which invokes nu(a) > max(nu(m), nu(c)).

Record 78 of 247

INTERPRETATION OF THE UNPRECEDENTEDLY LONG-LIVED HIGH-ENERGY EMISSION OF GRB 130427A

Liu, Ruo-Yu; Wang, Xiang-Yu; Wu, Xue-Feng


卷: 773; 期: 2; 页: L20-1-L20-5

High-energy photons (>100 MeV) are detected by the Fermi/Large Area Telescope from GRB 130427A up to almost one day after the burst, with an extra hard spectral component discovered in the high-energy afterglow. We show that this hard spectral component arises from afterglow synchrotron self-Compton (SSC) emission. This scenario can explain the origin of >10 GeV photons detected up to similar to 30,000 s after the burst, which would be difficult to explain via synchrotron radiation due to the limited maximum synchrotron photon energy. The lower energy multi-wavelength afterglow data can be fitted simultaneously by the afterglow


48

synchrotron emission. The implication of detecting the SSC emission for the circumburst environment is discussed.

Record 79 of 247

MULTIPOLE GRAVITATIONAL LENSING AND HIGH-ORDER PERTURBATIONS ON THE QUADRUPOLE LENS

Chu, Z.; Lin, W. P.; Li, G. L.; Kang, X.


卷: 765; 期: 2; 页: 134-1-134-10

An arbitrary surface mass density of the gravitational lens can be decomposed into multipole components. We simulate the ray tracing for the multipolar mass distribution of the generalized Singular Isothermal Sphere model based on deflection angles, which are analytically calculated. The magnification patterns in the source plane are then derived from an inverse shooting technique. As has been found, the caustics of odd mode lenses are composed of two overlapping layers for some lens models. When a point source traverses this kind of overlapping caustics, the image numbers change by +/- 4, rather than +/- 2. There are two kinds of caustic images. One is the critical curve and the other is the transition locus. It is found that the image number of the fold is exactly the average value of image numbers on two sides of the fold, while the image number of the cusp is equal to the smaller one. We also focus on the magnification patterns of the quadrupole (m = 2) lenses under the perturbations of m = 3, 4, and 5 mode components and found that one, two, and three butterfly or swallowtail singularities can be produced, respectively. With the increasing intensity of the high-order perturbations, the singularities grow up to bring sixfold image regions. If these perturbations are large enough to let two or three of the butterflies or swallowtails make contact, then eightfold or tenfold image regions can be produced as well. The possible astronomical applications are discussed.

Record 80 of 247

EARLY AFTERGLOWS OF GAMMA-RAY BURSTS IN A STRATIFIED MEDIUM WITH A POWER-LAW DENSITY DISTRIBUTION

Yi, Shuang-Xi; Wu, Xue-Feng; Dai, Zi-Gao


卷: 776; 期: 2; 页: 120-1-120-15

A long-duration gamma-ray burst (GRB) has been widely thought to arise from the collapse of a massive star, and it has been suggested that its ambient medium is a homogenous interstellar medium (ISM) or a stellar wind. There are two shocks when an ultra-relativistic fireball that has been ejected during the prompt gamma-ray emission phase sweeps up the circumburst medium: a reverse shock that propagates into the fireball, and a forward shock that propagates into the ambient medium. In this paper, we investigate the temporal evolution of the dynamics and emission of these two shocks in an environment with a general density distribution of n proportional to R-k (where R is the radius) by considering thick-shell and thin-shell cases. A GRB afterglow with one smooth onset peak at early times is understood to result from such external shocks. Thus, we can determine the medium density distribution by fitting the onset peak appearing in the light curve of an early optical afterglow. We apply our model to 19 GRBs and find that their k values are in the range of 0.4-1.4, with a typical value of k similar to 1, implying that this environment is neither a homogenous ISM with k = 0 nor a typical stellar wind with k = 2. This shows that the progenitors of these GRBs might have undergone a new mass-loss evolution.

Record 81 of 247

DELAYED ENERGY INJECTION MODEL FOR GAMMA-RAY BURST AFTERGLOWS

Geng, Jin Jun; Wu, Xue-Feng; Huang, Yong-Feng; Yu, Yong-Bo

Astrophysical Journal

卷: 779; 期: 1; 页: 28-1-28-20

The shallow decay phase and flares in the afterglows of gamma-ray bursts (GRBs) are widely believed to be associated with the later activation of the central engine. Some models of energy injection involve a continuous energy flow since the GRB trigger time, such as the magnetic dipole radiation from a magnetar. However, in the scenario involving a black hole accretion system, the energy flow from the fall-back accretion may be delayed for a fall-back time ~tfb. Thus, we propose a delayed energy injection model. The delayed energy would cause a notable rise to the Lorentz factor of the external shock, which will "generate" a bump in the multiple band afterglows. If the delayed time is very short, our model degenerates to the previous models. Our


49

model can explain the significant re-brightening in the optical and infrared light curves of GRB 081029 and GRB 100621A. A considerable fall-back mass is needed to provide the later energy; this indicates that GRBs accompanied with fall-back material may be associated with a low energy supernova so that the fraction of the envelope can survive during eruption. The fall-back time can give meaningful information on the properties of GRB progenitor stars.

Record 82 of 247

TURBULENCE IN THE INTERGALACTIC MEDIUM: SOLENOIDAL AND DILATATIONAL MOTIONS AND THE IMPACT OF NUMERICAL VISCOSITY

Zhu, Weishan; Feng, Long-long; Xia, Yinhua; Shu, Chi-Wang; Gu, Qiusheng; Fang, Li-Zhi


卷: 777; 期: 1; 页: 48-1-48-17

We use a suite of cosmological hydrodynamical simulations, run by two fixed grid codes, to investigate the properties of solenoidal and dilatational motions of the intergalactic medium (IGM) and the impact of numerical viscosity on turbulence in an Lambda CDM universe. The codes differ only in the spatial difference discretization. We find that (1) The vortical motion grows rapidly since z = 2 and reaches similar to 10 km s(-1)-90 km s(-1) at z = 0. Meanwhile, the small-scale compressive ratio r(CS) drops from 0.84 to 0.47, indicating comparable vortical and compressive motions at z = 0. (2) Power spectra of the solenoidal velocity possess two regimes, proportional to k(-0.89) and proportional to k(-2.02), while the total and dilatational velocity follow the scaling k(-1.88) and k(-2.20), respectively, in the turbulent range. The IGM turbulence may contain two distinct phases, the supersonic and post-supersonic phases. (3) The non-thermal pressure support, measured by the vortical kinetic energy, is comparable with the thermal pressure for rho(b) similar or equal to 10-100, or T < 10(5.5) Kat z = 0.0. The deviation of the baryon fraction from the cosmic mean shows a preliminary positive correlation with the turbulence pressure support. (4) A relatively higher numerical viscosity would dissipate both the compressive and vortical motions of the IGM into thermal energy more effectively, resulting in less developed vorticity, remarkably shortened inertial range, and leading to a non-negligible uncertainty in the thermal history of gas accretion.

Shocks in regions outside of clusters are significantly suppressed by numerical viscosity since z = 2, which may directly cause the different levels of turbulence between the two codes.

Record 83 of 247

Evidence for Two Distinct Populations of Type Ia Supernovae

Wang, Xiaofeng; Wang, Lifan; Filippenko, Alexei V.; Zhang, Tianmeng; Zhao, Xulin

SCIENCE

卷: 340; 期: 6129; 页: 170-173

Type Ia supernovae (SNe Ia) have been used as excellent standardizable candles for measuring cosmic expansion, but their progenitors are still elusive. Here, we report that the spectral diversity of SNe Ia is tied to their birthplace environments. We found that those with high-velocity ejecta are substantially more concentrated in the inner and brighter regions of their host galaxies than are normal-velocity SNe Ia. Furthermore, the former tend to inhabit larger and more luminous hosts. These results suggest that high-velocity SNe Ia likely originate from relatively younger and more metal-rich progenitors than do normal-velocity SNe Ia and are restricted to galaxies with substantial chemical evolution.

Record 84 of 247

IMAGE ANALYSIS FOR COSMOLOGY: RESULTS FROM THE GREAT10 STAR CHALLENGE

Kitching, T. D.; Rowe, B.; Gill, M.; Heymans, C.; Massey, R.; Witherick, D.; Courbin, F.; Georgatzis, K.; Gentile, M.; Gruen, D.; Kilbinger, M.; Li, G. L.; Mariglis, A. P.; Meylan, G.; Storkey, A.; Xin, B.

ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES

卷: 205; 期: 2; 页: 12-1-12-11

We present the results from the first public blind point-spread function (PSF) reconstruction challenge, the GRavitational lEnsing Accuracy Testing 2010 (GREAT10) Star Challenge. Reconstruction of a spatially varying PSF, sparsely sampled by stars, at non-star positions is a critical part in the image analysis for weak lensing where inaccuracies in the modeled ellipticity e and size R-2 can impact the ability to measure the shapes of galaxies. This is of importance because weak lensing is a particularly sensitive probe of dark energy and can be used to map the mass distribution of large scale structure. Participants in


50

the challenge were presented with 27,500 stars over 1300 images subdivided into 26 sets, where in each set a category change was made in the type or spatial variation of the PSF. Thirty submissions were made by nine teams. The best methods reconstructed the PSF with an accuracy of sigma(e) approximate to 2.5 x 10(-4) and sigma(R-2)/R-2 approximate to 7.4 x 10(-4). For a fixed pixel scale, narrower PSFs were found to be more difficult to model than larger PSFs, and the PSF reconstruction was severely degraded with the inclusion of an atmospheric turbulence model (although this result is likely to be a strong function of the amplitude of the turbulence power spectrum).

Record 85 of 247

Possible high-energy neutrino and photon signals from gravitational wave bursts due to double neutron star mergers

Gao, He; Zhang, Bing; Wu, Xue-Feng; Dai, Zi-Gao

PHYSICAL REVIEW D

卷: 88; 期: 4; 页: 43010-1-43010-6

As the technology of gravitational-wave and neutrino detectors becomes increasingly mature, a multimessenger era of astronomy is ushered in. Advanced gravitational-wave detectors are close to making a ground-breaking discovery of gravitational-wave bursts (GWBs) associated with mergers of double neutron stars (NS-NS). It is essential to study the possible electromagnetic and neutrino emission counterparts of these GWBs. Recent observations and numerical simulations suggest that at least a fraction of NS-NS mergers may leave behind a massive millisecond magnetar as the merger product. Here we show that protons accelerated in the forward shock powered by a magnetar wind pushing the ejecta launched during the merger process would interact with photons generated in the dissipating magnetar wind and emit high-energy neutrinos and photons. We estimate the typical energy and fluence of the neutrinos from such a scenario. We find that similar to PeV neutrinos could be emitted from the shock front as long as the ejecta could be accelerated to a relativistic speed. The diffuse neutrino flux from these events, even under the most optimistic scenarios, is too low to account for the two events announced by the IceCube Collaboration, but it is only slightly lower than the diffuse flux of GRBs, making it an important candidate for the diffuse background of

similar to PeV neutrinos. The neutron-pion decay of these events make them a moderate contributor to the sub-TeV gamma-ray diffuse background.

Record 86 of 247

A COMPREHENSIVE STUDY OF GAMMA-RAY BURST OPTICAL EMISSION. II. AFTERGLOW ONSET AND LATE RE-BRIGHTENING COMPONENTS

Liang, En-Wei; Li, Liang; Gao, He; Zhang, Bing; Liang, Yun-Feng; Wu, Xue-Feng; Yi, Shuang-Xi; Dai, Zi-Gao; Tang, Qing-Wen; Chen, Jie-Min; Lu, Hou-Jun; Zhang, Jin; Lu, Rui-Jing; Lu, Lian-Zhong; Wei, Jian-Yan


卷: 774; 期: 1; 页: 13-1-13-16

We continue our systematic statistical study of various components of gamma-ray burst (GRB) optical light curves. We decompose the early onset bump and the late re-brightening bump with empirical fits and analyze their statistical properties. Among the 146 GRBs that have well-sampled optical light curves, the onset and re-brightening bumps are observed in 38 and 26 GRBs, respectively. It is found that the typical rising and decaying slopes for both the onset and re-brightening bumps are similar to 1.5 and similar to-1.15, respectively. No early onset bumps in the X-ray band are detected to be associated with the optical onset bumps, while an X-ray re-brightening bump is detected for half of the re-brightening optical bumps. The peak luminosity is anti-correlated with the peak time L-p proportional to t(p)(-1.81 +/- 0.32) for the onset bumps and L-p proportional to t(p)(-0.83 +/- 0.17) for the re-brightening bumps. Both L-p and the isotropic energy release of the onset bumps are correlated with E-gamma,E- iso, whereas no similar correlation is found for the re-brightening bumps. These results suggest that the afterglow onset bumps are likely due to the deceleration of the GRB fireballs. Taking the onset bumps as probes for the properties of the fireballs and their ambient medium, we find that the typical power-law index of the relativistic electrons is 2.5 and the medium density profile behaves as n proportional to r(-1) within the framework of the synchrotron external shock models. With the medium density profile obtained from our analysis, we also confirm the correlation between the initial Lorentz factor (Gamma(0)) and


51

E-iso,E-gamma in our previous work. The jet component that produces the re-brightening bump seems to be on-axis and independent of the prompt emission jet component. Its typical kinetic energy budget would be about one order of magnitude larger than the prompt emission component, but with a lower Gamma(0), typically several tens.

Record 87 of 247

Further evidence for the accretion disc origination of the double-peaked broad H alpha of 3C 390.3

Zhang, Xue-Guang


卷: 431; 期: 1; 页: L112-L116

In this Letter, under the widely accepted theoretical accretion disc model for the double-peaked emitter 3C 390.3, the extended disc-like broad-line region can be well split into 10 rings, and then the time lags between the lines from the rings and the continuum emission are estimated, based on the observed spectra around 1995. We can find one very strong correlation between the determined time lags (in units of light-day) and the flux-weighted radii (in units of R-G) of the rings, which is well consistent with the expected results through the theoretical accretion disc model. Moreover, through the strong correlation, the black hole masses of 3C 390.3 are independently estimated as similar to 10(9)M(circle dot), the same as the reported black hole masses in the literature. The consistencies provide further evidence to strongly support the accretion disc origination of the double-peaked broad Balmer lines of 3C 390.3.

Record 88 of 247

Optical spectral index-luminosity relation for the 17 mapped Palomar-Green quasars

Zhang, Xue-Guang


卷: 435; 期: 3; 页: 2141-2151

In this paper, the optical spectra index-luminosity relationship is checked for the well-known 17 individually mapped quasi-stellar objects (QSOs), in order to give one more clearer conclusion on the so far conflicting dependence of the spectral

index on the luminosity for an active galactic nucleus (AGN). Unlike the global relationships based on the colour difference (photometry parameters) for samples of AGNs, a more reliable relationship is determined for the multi-epoch observed individually mapped QSOs with no contamination from the host galaxies, the line variabilities and the very different central properties. The final confirmed results are as follows. (i) No strong dependence of the optical spectral index on the continuum luminosity can be found for all 17 QSOs, besides two objects (PG 0026 and PG 1613) that have some weak trends (with 3 Sigma confidence level) for the relationship. In other words, the common expectation that 'AGNs get bluer when they get brighter' is not so common. (ii) There are very different damped intrinsic variability time-scales for the variability modes of the optical spectral index and the continuum emission, through the well-applied damped random walk method for the AGN variability. In other words, there are some different intrinsic mechanisms controlling the variabilities of the optical spectral index and the power-law AGN continuum emission. Therefore, the much weaker dependence of the optical spectral index on the continuum luminosity can be further confirmed.

Record 89 of 247

More evidence for the intermediate broad line region of the mapped AGN PG 0052+251

Zhang, Xue-Guang


卷: 434; 期: 3; 页: 2664-2678

In this paper, the properties of the proposed intermediate broad emission line region (BLR) are checked for the mapped AGN PG 0052+251. With the considerations of the apparent effects of the broad He ii line on the observed broad H beta profile, the line parameters (especially the line width and the line flux) of the observed broad H alpha and the broad H beta are carefully determined. Based on the measured line parameters, the model with two broad components applied for each observed broad Balmer line is preferred, and then confirmed by the calculated much different time lags for the inner/intermediate broad components and the corresponding virial black hole mass ratio determined by the properties of the inner and the


52

intermediate broad components. Then, the correlation between the broad line width and the broad line flux is checked for the two broad components: one clearly strong negative correlation for the inner broad component and one positive correlation for the intermediate broad component. The different correlations for the two broad components strongly support the intermediate BLR of PG 0052+251.

Record 90 of 247

Correlation between the line width and the line flux of the double-peaked broad H alpha of 3C390.3

Zhang, Xue-Guang


卷: 429; 期: 3; 页: 2274-2286

In this paper, we carefully check the correlation between the line width (second moment) and the line flux of the double-peaked broad H alpha of the well-known mapped active galactic nucleus (AGN) 3C390.3 in order to show some further distinctions between double-peaked emitters and normal broad-line AGN. Based on the virialization assumption M-BH proportional to R-BLR x V-2(BLR) and the empirical relation R-BLR proportional to L-similar to 0.5, one strong negative correlation between the line width and the line flux of the double-peaked broad lines should be expected for 3C390.3, such as the negative correlation confirmed for the mapped broad-line object NGC5548, R-BLR x V-2(BLR) proportional to L-similar to 0.5 x sigma(2) = constant. Moreover, based on the public spectra around 1995 from the AGN WATCH project for 3C390.3, one reliable positive correlation is found between the line width and the line flux of the double-peaked broad H alpha. In the context of the proposed theoretical accretion disc model for double-peaked emitters, the unexpected positive correlation can be naturally explained, due to different time delays for the inner and outer parts of the disc-like broad-line region (BLR) of 3C390.3. Moreover, the virialization assumption is checked and found to be still available for 3C390.3. However, the time-varying size of the BLR of 3C390.3 cannot be expected by the empirical relation R-BLR proportional to L-similar to 0.5. In other words, the mean size of the BLR of 3C390.3 can be estimated by the continuum luminosity (line luminosity), while the continuum emission

strengthening leads to the size of BLR decreasing (not increasing) in different moments for 3C390.3. Then, we compared our results of 3C390.3 with the previous results reported in the literature for the other double-peaked emitters, and found that before to clearly correct the effects from disc physical parameters varying (such as the effects of disc precession) for long-term observed line spectra, it is not so meaningful to discuss the correlation of the line parameters of double-peaked broad lines. Furthermore, due to the probable 'external' ionizing source with so far unclear structures, it is hard to give one conclusion that the positive correlation between the line width and the line flux can be found for all double-peaked emitters, even after the considerations of disc physical parameters varying. However, once one positive correlation of broad-line parameters is found, the accretion disc origination of the broad line should be considered first.

Record 91 of 247

GIANT X-RAY BUMP IN GRB 121027A: EVIDENCE FOR FALL-BACK DISK ACCRETION

Wu, Xue-Feng; Hou, Shu-Jin; Lei, Wei-Hua


卷: 767; 期: 2; 页: L36-1-L36-5

A particularly interesting discovery in observations of GRB 121027A is that of a giant X-ray bump detected by the Swift/X-Ray Telescope. The X-ray afterglow re-brightens sharply at similar to 10(3) s after the trigger by more than two orders of magnitude in less than 200 s. This X-ray bump lasts for more than 10(4) s. It is quite different from typical X-ray flares. In this Letter we propose a fall-back accretion model to interpret this X-ray bump within the context of the collapse of a massive star for a long-duration gamma-ray burst. The required fall-back radius of similar to 3.5x10(10) cm and mass of similar to 0.9-2.6M(circle dot) imply that a significant part of the helium envelope should survive through the mass loss during the last stage of the massive progenitor of GRB 121027A.

Record 92 of 247

The Gamma-Ray Burst Hubble Diagram and Its Implications for Cosmology

Wei, Jun-Jie; Wu, Xue-Feng; Melia, Fulvio



53

卷: 772; 期: 1; 页: 43-1-43-11

In this paper, we continue to build support for the proposal to use gamma-ray bursts (GRBs) as standard candles in constructing the Hubble diagram at redshifts beyond the current reach of Type Ia supernova observations. We confirm that correlations among certain spectral and light-curve features can indeed be used as luminosity indicators, and demonstrate from the most up-to-date GRB sample appropriate for this work that the Lambda CDM model optimized with these data is characterized by parameter values consistent with those in the concordance model. Specifically, we find that (Omega(m), Omega(Lambda)) approximate to (0.25(-0.06)(+0.05), 0.75(-0.05)(+0.06)), which are consistent, to within 1 sigma, with (0.29, 0.71) obtained from the 9 yr Wilkinson Microwave Anisotropy Probe data. We also carry out a comparative analysis between Lambda CDM and the R-h = ct universe and find that the optimal Lambda CDM model fits the GRB Hubble diagram with a reduced chi(2)(dof) approximate to 2.26, whereas the fit using R-h = ct results in a chi(2)(dof) approximate to 2.14. In both cases, about 20% of the events lie at least 2 sigma away from the best-fit curves, suggesting that either some contamination by non-standard GRB luminosities is unavoidable or that the errors and intrinsic scatter associated with the data are being underestimated. With these optimized fits, we use three statistical tools-the Akaike information criterion, the Kullback information criterion, and the Bayes information criterion-to show that, based on the GRB Hubble diagram, the likelihood of R-h = ct being closer to the correct model is similar to 85%-96%, compared to similar to 4%-15% for Lambda CDM.

Record 93 of 247

Bright Broadband Afterglows of Gravitational Wave Bursts from Mergers of Binary Neutron Stars

Gao, He; Ding, Xuan; Wu, Xue-Feng; Zhang, Bing; Dai, Zi-Gao


卷: 771; 期: 2; 页: 86-1-86-8

If double neutron star mergers leave behind a massive magnetar rather than a black hole, then a bright early afterglow can follow the gravitational wave burst (GWB) even if there is no short gamma-ray burst (SGRB)-GWB association or if

there is an association but the SGRB does not beam toward Earth. Besides directly dissipating the proto-magnetar wind, as suggested by Zhang, here we suggest that the magnetar wind could push the ejecta launched during the merger process and, under certain conditions, would reach a relativistic speed. Such a magnetar-powered ejecta, when interacting with the ambient medium, would develop a bright broadband afterglow due to synchrotron radiation. We study this physical scenario in detail and present the predicted X-ray, optical, and radio light curves for a range of magnetar and ejecta parameters. We show that the X-ray and optical light curves usually peak around the magnetar spin-down timescale (similar to 10(3)-10(5) s), reaching brightnesses readily detectable by wide-field X-ray and optical telescopes, and remain detectable for an extended period. The radio afterglow peaks later, but is much brighter than the case without a magnetar energy injection. Therefore, such bright broadband afterglows, if detected and combined with GWBs in the future, would be a probe of massive millisecond magnetars and stiff equations of state for nuclear matter.

Record 94 of 247

Is There a Relation between Duration and Eiso in Gamma-Ray Bursts?

Hou, Shu-Jin; Liu, Tong; Lin, Da-Bin; Wu, Xue-Feng; Lu, Ju-Fu

Proceedings of the International Astronomical Union, IAU Symposium

卷: 290; 期: 1; 页: 223-224

The system of accretion disk and black hole is usually considered as the central engine of Gamma-ray Bursts (GRBs). It is usually thought that the disk in the central engine of GRBs is the advection-dominated accretion disk, which is developed from a massive (mass Mdisk) torus at radius rdisk. We find a positive correlation between the isotropic gamma-ray energy Eiso and duration (so-called T90) for GRBs. We interpret this correlation within the advection-dominated accretion disk model, associating Eiso and T90 with Mdisk and viscous timescale respectively.

Record 95 of 247

Shape measurement by using basis functions

Li, Guoliang; Xin, Bo; Cui, Wei


54

IAU Symposium

卷: 8; 期: S288; 页: 306-308

Gravitational lensing is one of most promising tools to probe dark energy and dark matter in our Universe. Lensing by larger-scale structures distorts the shape of background galaxies. For ground-based observations the shape is further distorted by atmospheric turbulence and optical distortions. Many algorithms were proposed to measure the shear signal but the systematic biases are still too large to be acceptable for the larger-sky surveys in the future. I will present our new algorithms for PSF reconstruction and shape measurements based on several sets of basis functions.

Record 96 of 247

PHOTOMETRY OF VARIABLE STARS FROM DOME A, ANTARCTICA: RESULTS FROM THE 2010 OBSERVING SEASON

Wang, Lingzhi; Macri, Lucas M.; Wang, Lifan; Ashley, Michael C. B.; Cui, Xiangqun; Peng, Long-Long; Gong, Xuefei; Lawrence, Jon S.; Liu, Qiang; Daniel Luong-Van; Pennypacker, Carl R.; Shang, Zhaohui; Storey, John W. V.; Yang, Huigen; Yang, Ji; Yuan, Xiangyan; York, Donald G.; Zhou, Xu; Zhu, Zhenxi; Zhu, Zonghong

ASTRONOMICAL JOURNAL

卷: 146; 期: 6; 页: 1-14

We present results from a season of observations with the Chinese Small Telescope ARray, obtained over 183 days of the 2010 Antarctic winter. We carried out high-cadence time-series aperture photometry of 9125 stars with i less than or similar to 15.3 mag located in a 23 deg(2) region centered on the south celestial pole. We identified 188 variable stars, including 67 new objects relative to our 2008 observations, thanks to broader synoptic coverage, a deeper magnitude limit, and a larger field of view. We used the photometric data set to derive site statistics from Dome A. Based on two years of observations, we find that extinction due to clouds at this site is less than 0.1 and 0.4 mag during 45% and 75% of the dark time, respectively.

Record 97 of 247

Discovery Of An Extra Hard Spectral Component In The High-Energy Afterglow Emission Of GRB 130427A

Tam, Pak-Hin Thomas ; Tang, Qing-Wen ; Hou,

Shu-Jin ;Liu, Ruo-Yu; Wang, Xiang-Yu


卷:771;期:1;页: L13(1-5)

The extended high-energy gamma-ray (> 100 MeV) emission which occurs after prompt gamma-ray bursts (GRBs) is usually characterized by a single power-law spectrum, which has been explained as the afterglow synchrotron radiation. The afterglow inverse Compton emission has long been predicted to be able to produce a high-energy component as well, but previous observations have not clearly revealed such a signature, probably due to the small number of > 10 GeV photons even for the brightest GRBs known so far. In this Letter, we report on the Fermi Large Area Telescope observations of the > 100 MeV emission from the very bright and nearby GRB130427A. We characterize the time-resolved spectra of the GeV emission from the GRB onset to the afterglow phase. By performing time-resolved spectral fits of GRB130427A, we found strong evidence of an extra hard spectral component that exists in the extended high-energy emission of this GRB. We argue that this hard component may arise from the afterglow inverse Compton emission.

Record 98 of 247

The dependence of tidal stripping efficiency on the satellite and host galaxy morphology

Chang, Jiang; Maccio, Andrea V.; Kang, Xi


卷: 431; 期: 4; 页: 3533-3542

In this paper, we study the tidal stripping process for satellite galaxies orbiting around a massive host galaxy, and focus on its dependence on the morphology of both satellite and host galaxy. For this purpose, we use three different morphologies for the satellites: pure disc, pure bulge and a mixture bulge+disc. Two morphologies are used for the host galaxies: bulge+disc and pure bulge. We find that while the spheroidal stellar component experiences a constant power law like mass removal, the disc is exposed to an exponential mass-loss when the tidal radius of the

Galaxy Cosmology and Dark Energy


55

satellite is of the same order of the disc scalelength. This dramatic mass-loss is able to completely remove the stellar component on time-scale of 100 Myr. As a consequence two satellites with the same stellar and dark matter masses, on the same orbit could either retain considerable fraction of their stellar mass after 10 Gyr or being completely destroyed, depending on their initial stellar morphology. We find that there are two characteristic time-scales describing the beginning and the end of the disc removal, whose values are related to the size of the disc. This result can be easily incorporated in semi-analytical models. We also find that the host morphology and the orbital parameters also have an effect on determining the mass removal, but they are of secondary importance with respect to satellite morphology. We conclude that satellite morphology has a very strong effect on the efficiency of stellar stripping and should be taken into account in modelling galaxy formation and evolution.

Record 99 of 247

THE EFFECT OF WARM DARK MATTER ON GALAXY PROPERTIES: CONSTRAINTS FROM THE STELLAR MASS FUNCTION AND THE TULLY-FISHER RELATION

Kang, Xi; Maccio, Andrea V.; Dutton, Aaron A.


卷: 767; 期: 1; 页: 22-1-22-7

In this paper, we combine high-resolution N-body simulations with a semi-analytical model of galaxy formation to study the effects of a possible warm dark matter (WDM) component on the observable properties of galaxies. We compare three WDM models with a dark matter (DM) mass of 0.5, 0.75, and 2.0 keV with the standard cold dark matter case. For a fixed set of parameters describing the baryonic physics, the WDM models predict fewer galaxies at low (stellar) masses, as expected due to the suppression of power on small scales, while no substantial difference is found at the high-mass end. However, these differences in the stellar mass function vanish when a different set of parameters is used to describe the (largely unknown) galaxy formation processes. We show that it is possible to break this degeneracy between DM properties and the parameterization of baryonic physics by combining observations on the stellar mass function with the Tully-Fisher relation (the relation between stellar mass and

the rotation velocity at large galactic radii as probed by resolved H I rotation curves). WDM models with a too warm candidate (m(nu) < 0.75 keV) cannot simultaneously reproduce the stellar mass function and the Tully-Fisher relation. We conclude that accurate measurements of the galaxy stellar mass function and the link between galaxies and DM halos down to the very low mass end can give very tight constraints on the nature of DM candidates.

Record 100 of 247

Alignments Of Galaxies Within Cosmic Filaments From SDSS DR7

Zhang, Youcai ; Yang, Xiaohu; Wang, Huiyuan; Wang, Lei;Mo, H. J.; van den Bosch, Frank C.


卷:779;期:2;页: 160(1-10)

Using a sample of galaxy groups selected from the Sloan Digital Sky Survey Data Release 7, we examine the alignment between the orientation of galaxies and their surrounding large-scale structure in the context of the cosmic web. The latter is quantified using the large-scale tidal field, reconstructed from the data using galaxy groups above a certain mass threshold. We find that the major axes of galaxies in filaments tend to be preferentially aligned with the directions of the filaments, while galaxies in sheets have their major axes preferentially aligned parallel to the plane of the sheets. The strength of this alignment signal is strongest for red, central galaxies, and in good agreement with that of dark matter halos in N-body simulations. This suggests that red, central galaxies are well aligned with their host halos, in quantitative agreement with previous studies based on the spatial distribution of satellite galaxies. There is a luminosity and mass dependence that brighter and more massive galaxies in filaments and sheets have stronger alignment signals. We also find that the orientation of galaxies is aligned with the eigenvector associated with the smallest eigenvalue of the tidal tensor. These observational results indicate that galaxy formation is affected by large-scale environments and strongly suggest that galaxies are aligned with each other over scales comparable to those of sheets and filaments in the cosmic web.


56

Record 101 of 247

A Herschel Spectroscopic Survey of Warm Molecular Gas in Local Luminous Infrared Galaxies

Lu, Nanyao; Xu, C. K.; Gao, Y.; Isaak, K.; Armus, L.; Appleton, P.; Charmandaris, V.; Díaz-Santos, T.; Evans, A.; Howell, J.; Iwasawa, K.; Leech, J.; Lord, S.; Mazzarella, J.; Petric, A.; Sanders, D.; Schulz, B.; Surace, J.; van der Werf, P.; Zhao, Y.

Astronomical Society of the Pacific Conference Series

卷: 477; 页: 31-35

We describe an on-going Herschel 200–700 μm spectroscopic survey of a flux-limited sample of 125 local luminous infrared galaxies (LIRGs), targeting primarily at CO line emission from warm and dense molecular gas. The program will provide important statistical data on the interplay between warm molecular gas, IR luminosity, star formation rate and efficiency, AGN, and the diverse properties of LIRGs. Of the 30 sample galaxies observed so far (18 by us; 12 taken from Herschel archive), about 15% show a dominant or significant hot CO gas component emitting at J > 10, that is likely heated by AGN. The other 85% is dominated by a warm gas component with CO line emission peaking at J ≤ 8, likely powered by starburst. While the spectral shapes of the warm gas component show little overall dependence on the total IR luminosity LIR, the relative contribution from the hot component appears to correlate positively with LIR. The tightest one-to-one correlation between CO line luminosity and LIR seems to be for CO(7-6), implying that the bulk of LIR should be correlated with warm molecular gas of such density and temperature that its CO line emission peaks around J ~ 7.

Record 102 of 247

The Star Formation Efficiency in Stephan's Quintet Intragroup Regions

Natale, G.; Tuffs, R. J.; Xu, C. K.; Popescu, C. C.; Fischera, J.; Lisenfeld, U.; Lu, N.; Appleton, P.; Dopita, M.; Duc, P.-A.; Gao, Y.; Reach, W.; Sulentic, J.; Yun, M.

Conference Proceedings "galaxy Mergers In An Evolving Universe"

卷: 477; 页: 73-76

We investigated the star formation efficiency for all the dust emitting sources in Stephan's Quintet (SQ). We inferred star formation rates using Spitzer MIR/FIR and GALEX FUV data and combined them with gas column density measurements by various authors, in order to position each source in a Kennicutt-Schmidt diagram. Our results show that the bright IGM star formation regions in SQ present star formation efficiencies consistent with those observed within local galaxies. On the other hand, star formation in the intergalactic shock region seems to be rather inhibited.

Record 103 of 247

The nature of [S III]lambda lambda 9096, 9532 emitters at z=1.34 and 1.23

An FangXia; Zheng XianZhong; Meng YanZhi; Chen Yang; Wen ZhangZheng; Lu GuoLiang

SCIENCE CHINA-PHYSICS MECHANICS & ASTRONOMY

卷: 56; 期: 11; 页: 2226-2235

A study of [S iii]lambda lambda 9096, 9532 emitters at z = 1.34 and 1.23 is presented using our deep narrow-band H (2) S 1 (centered at 2.13 mu m) imaging survey of the Extended Chandra Deep Field South (ECDFS). We combine our data with multi-wavelength data of ECDFS to build up spectral energy distributions (SEDs) from the U to the K (s)-band for emitter candidates selected with strong excess in H (2) S 1 - K (s) and derive photometric redshifts, line luminosities, stellar masses and extinction. A sample of 14 [S iii] emitters are identified with H (2) S 1 < 22.8 and K (s) < 24.8 (AB) over 381 arcmin(2) area, having [S iii] line luminosity L ([SIII]) =similar to 1041.5-42.6 erg s(-1). None of the [S iii] emitters is found to have X-ray counterpart in the deepest Chandra 4Ms observation, suggesting that they are unlikely powered by AGNs. The HST/ACS F606W and HST/WFC3 F160W images show their rest-frame UV and optical morphologies. About half of the [S iii] emitters are mergers and at least one third are disk-type galaxies. Nearly all [S iii] emitters exhibit a prominent Balmer break in their SEDs, indicating the presence of a significant post-starburst component. Taken together, our results imply that both shock heating in post-starburst and photoionization caused by young massive stars are likely to excite strong [S iii] emission lines. We conclude that the [S iii] emitters in our sample are dominated by star-forming galaxies (SFGs) with

Star Formation in Galaxies


57

stellar mass 8.7 < log(M/M (aS (TM))) < 9.9.

Record 104 of 247

H2O emission in high-z ultra-luminous infrared galaxies

Omont, A.; Yang, C.; Cox, P.; Neri, R.; Beelen, A.; Bussmann, R. S.; Gavazzi, R.; van der Werf, P.; Riechers, D.; Downes, D.; Krips, M.; Dye, S.; Ivison, R.; Vieira, J. D.; Weiss, A.; Aguirre, J. E.; Baes, M.; Baker, A. J.; Bertoldi, F.; Cooray, A.; Dannerbauer, H.; De Zotti, G.; Eales, S. A.; Fu, H.; Gao, Y.; Guelin, M.; Harris, A. I.; Jarvis, M.; Lehnert, M.; Leeuw, L.; Lupu, R.; Menten, K.; Michalowski, M. J.; Negrello, M.; Serjeant, S.; Temi, P.; Auld, R.; Dariush, A.; Dunne, L.; Fritz, J.; Hopwood, R.; Hoyos, C.; Ibar, E.; Maddox, S.; Smith, M. W. L.; Valiante, E.; Bock, J.; Bradford, C. M.; Glenn, J.; Scott, K. S.


卷: 551;页: A115-1-A115-12

Using the IRAM Plateau de Bure interferometer (PdBI), we report the detection of water vapor in six new lensed ultra-luminous starburst galaxies at high redshift, discovered in the Herschel Astrophysical Terahertz Large Area Survey (H-ATLAS). The sources are detected either in the 2(02)-1(11) or 2(11)-2(02) H2O emission lines with integrated line fluxes ranging from 1.8 to 14 Jy km s(-1). The corresponding apparent luminosities are mu L-H2O similar to 3-12 x 10(8) L-circle dot, where mu is the lensing magnification factor (3 < mu < 12). These results confirm that H2O lines are among the strongest molecular lines in high-z ultra-luminous starburst galaxies, with intensities almost comparable to those of the high-J CO lines, and similar profiles and line widths (similar to 200-900 km s(-1)). With the current sensitivity of the PdBI, the water lines can therefore easily be detected in high-z lensed galaxies (with F(500 mu m) > 100 mJy) discovered in the Herschel surveys. Correcting the luminosities for amplification, using existing lensing models, L-H2O is found to have a strong dependence on the infrared luminosity, varying as similar to L-IR(1.2). This relation, which needs to be confirmed with better statistics, may indicate a role of radiative (infrared) excitation of the H2O lines, and implies that high-z galaxies with L-IR greater than or similar to 10(13) L-circle dot tend to be very strong emitters in water vapor, that have no equivalent in the local universe.

Record 105 of 247

WATER VAPOR IN NEARBY INFRARED GALAXIES AS PROBED BY HERSCHEL

Yang, Chentao; Gao, Yu; Omont, A.; Liu, Daizhong; Isaak, K. G.; Downes, D.; van der Werf, P. P.; Lu, Nanyao


卷: 771; 期: 2; 页: L24-1-L24-6

We report the first systematic study of the submillimeter water vapor rotational emission lines in infrared (IR) galaxies based on the Fourier Transform Spectrometer (FTS) data of Herschel SPIRE. Among the 176 galaxies with publicly available FTS data, 45 have at least one H2O emission line detected. The H2O line luminosities range from similar to 1 x 10(5) L-circle dot to similar to 5 x 10(7) L-circle dot while the total IR luminosities (L-IR) have a similar spread (similar to 1-300 x 10(10) L-circle dot). In addition, emission lines of H2O+ and (H2O)-O-18 are also detected. H2O is found, for most galaxies, to be the strongest molecular emitter after CO in FTS spectra. The luminosity of the five most important H2O lines is near-linearly correlated with L-IR, regardless of whether or not strong active galactic nucleus signature is present. However, the luminosity of H2O(2(11)-2(02)) and H2O(2(20)-2(11)) appears to increase slightly faster than linear with L-IR. Although the slope turns out to be slightly steeper when z similar to 2-4 ULIRGs are included, the correlation is still closely linear. We find that L-H2O/L-IR decreases with increasing f(25)/f(60), but see no dependence on f(60)/f(100), possibly indicating that very warm dust contributes little to the excitation of the submillimeter H2O lines. The average spectral line energy distribution (SLED) of the entire sample is consistent with individual SLEDs and the IR pumping plus collisional excitation model, showing that the strongest lines are H2O(2(02)-1(11)) and H2O(3(21)-3(12)).

Record 106 of 247

A SiO 2-1 SURVEY TOWARD GAS-RICH ACTIVE GALAXIES

Wang, Junzhi; Zhang, Jiangshui; Shi, Yong; Zhang, Zhiyu


卷: 778; 期: 2; 页: L39-1-L39-5

In order to study the feedback from active galactic nuclei (AGNs), we performed a survey of SiO J = 2-1 (v = 0) transition toward ten gas-rich active galaxies with the IRAM 30 m telescope. As the first survey of SiO in such galaxies, we detected SiO J =


58

2-1 (v = 0) emission in six galaxies above the 3 sigma level and one galaxy (NGC 3690) at the 2.7 sigma level. The detection rate is not related to the AGN type or to star formation activity. In comparison with M82, which is a pure star-forming galaxy without nuclear activity, our SiO detections could not be completely ascribed to being due to star formation activity. This suggests that the AGN feedback may be efficient in producing SiO molecules in such galaxies. Further surveys with large single-dish millimeter telescopes and interferometers are necessary for understanding the origin of SiO in galaxies with nuclear activity.

Record 107 of 247

High resolution observations of the 6 cm H2CO maser in NGC 6240

Wang, Jun-Zhi; Zhang, Zhi-Yu; Gao, Yu


卷: 13; 期: 3; 页: 270-276

We present high resolution (similar to 1 '') H2CO maser and 5 GHz radio continuum observations toward nearby merging galaxy NGC 6240 made with the Very Large Array in an A configuration. Two concentrations of H2CO emission at about a 6 sigma level have been detected, one of which is associated with the strongest CO peak in the overlap region while the other is about 2 '' southwest of the southern galaxy. Both H2CO concentrations are associated with near infrared H-2 emission, which is thought to be from shocked molecular gas. The total H2CO line luminosity in NGC 6240 is about 60% of that in Arp 220. Based on the distribution of H2CO emission in NGC 6240, which has both active galactic nuclei and an extreme starburst, the H2CO megamaser is likely to be related to the effect of the starburst instead of nuclear activity. Radio continuum cannot be the inversion mechanism of H2CO megamasers, because the two H2CO concentrations in NGC 6240 are not associated with radio continuum emission. Instead, with the association of near infrared H-2 emission, shock dynamics may produce the inverted population of H2CO needed to generate megamasers.

Record 108 of 247

SHOCK-ENHANCED C+ EMISSION AND THE DETECTION OF H2O FROM THE STEPHAN'S QUINTET GROUP-WIDE SHOCK USING HERSCHEL

Appleton, P. N.; Guillard, P.; Boulanger, F.; Cluver,

M. E.; Ogle, P.; Falgarone, E.; des Forets, G. Pineau; O'Sullivan, E.; Duc, P. -A.; Gallagher, S.; Gao, Y.; Jarrett, T.; Konstantopoulos, I.; Lisenfeld, U.; Lord, S.; Lu, N.; Peterson, B. W.; Struck, C.; Sturm, E.; Tuffs, R.; Valchanov, I.; van der Werf, P.; Xu, K. C.


卷: 777; 期: 1; 页: 66-1-66-16

We present the first Herschel spectroscopic detections of the [O I] 63 mu m and [C II] 158 mu m fine-structure transitions, and a single para-H2O line from the 35 x 15 kpc(2) shocked intergalactic filament in Stephan's Quintet. The filament is believed to have been formed when a high-speed intruder to the group collided with a clumpy intergroup gas. Observations with the PACS spectrometer provide evidence for broad (>1000 km s(-1)) luminous [C II] line profiles, as well as fainter [O I] 63 mu m emission. SPIRE FTS observations reveal water emission from the p-H2O (1(11)-0(00)) transition at several positions in the filament, but no other molecular lines. The H2O line is narrow and may be associated with denser intermediate-velocity gas experiencing the strongest shock-heating. The [C II]/PAH(tot) and [C II]/FIR ratios are too large to be explained by normal photo-electric heating in photodissociation regions. H II region excitation or X-ray/cosmic-ray heating can also be ruled out. The observations lead to the conclusion that a large fraction the molecular gas is diffuse and warm. We propose that the [C II], [O I], and warm H-2 line emission is powered by a turbulent cascade in which kinetic energy from the galaxy collision with the intergalactic medium is dissipated to small scales and low velocities, via shocks and turbulent eddies. Low-velocity magnetic shocks can help explain both the [C II]/[O I] ratio, and the relatively high [C II]/H-2 ratios observed. The discovery that [C II] emission can be enhanced, in large-scale turbulent regions in collisional environments, has implications for the interpretation of [C II] emission in high-z galaxies.

Record 109 of 247

Evidence for CO Shock Excitation in NGC 6240 from Herschel SPIRE Spectroscopy

Meijerink, R.; Kristensen, L. E.; Weiss, A.; van der Werf, P. P.; Walter, F.; Spaans, M.; Loenen, A. F.; Fischer, J.; Israel, F. P.; Isaak, K.; Papadopoulos, P. P.; Aalto, S.; Armus, L.; Charmandaris, V.; Dasyra, K. M.; Diaz-Santos, T.; Evans, A.; Gao, Y.; Gonzalez-Alfonso, E.; Guesten, R.; Henkel, C.;


59

Kramer, C.; Lord, S.; Martin-Pintado, J.; Naylor, D.; Sanders, D. B.; Smith, H.; Spinoglio, L.; Stacey, G.; Veilleux, S.; Wiedner, M. C.


卷: 762; 期: 2; 页: L16-1-L16-5

We present Herschel SPIRE FTS spectroscopy of the nearby luminous infrared galaxy NGC 6240. In total 20 lines are detected, including CO J = 4-3 through J = 13-12, 6 H2O rotational lines, and [C I] and [N II] fine-structure lines. The CO to continuum luminosity ratio is 10 times higher in NGC 6240 than Mrk 231. Although the CO ladders of NGC 6240 and Mrk 231 are very similar, UV and/or X-ray irradiation are unlikely to be responsible for the excitation of the gas in NGC 6240. We applied both C and J shock models to the H-2 v = 1-0 S(1) and v = 2-1 S(1) lines and the CO rotational ladder. The CO ladder is best reproduced by a model with shock velocity v(s) = 10 km s(-1) and a pre-shock density n(H) = 5 x 10(4) cm(-3). We find that the solution best fitting the H-2 lines is degenerate. The shock velocities and number densities range between v(s) = 17-47 km s(-1) and n(H) = 10(7)-5x10(4) cm(-3), respectively. The H-2 lines thus need a much more powerful shock than the CO lines. We deduce that most of the gas is currently moderately stirred up by slow (10 km s(-1)) shocks while only a small fraction (less than or similar to 1%) of the interstellar medium is exposed to the high-velocity shocks. This implies that the gas is rapidly losing its highly turbulent motions. We argue that a high CO line-to-continuum ratio is a key diagnostic for the presence of shocks.

Record 110 of 247

MULTI-WAVELENGTH STUDY OF A COMPLETE IRAC 3.6 mu m SELECTED GALAXY SAMPLE: A FAIR CENSUS OF RED AND BLUE POPULATIONS AT REDSHIFTS 0.4-1.2

Huang, J-S; Faber, S. M.; Willmer, C. N. A.; Rigopoulou, D.; Koo, D.; Newman, J.; Shu, C.; Ashby, M. L. N.; Barmby, P.; Coil, A.; Luo, Z.; Magdis, G.; Wang, T.; Weiner, B.; Willner, S. P.; Zheng, X. Z.; Fazio, G. G.


卷: 766; 期: 1; 页: 21-1-21-17

We present a multi-wavelength study of a 3.6 mu m selected galaxy sample in the Extended Groth Strip (EGS). The sample is complete for galaxies with stellar mass >10(9.5) M-circle dot and redshift 0.4 < z < 1.2. In this redshift range, the Infrared Array Camera 3.6 mu m band measures

the rest-frame near-infrared band, permitting nearly unbiased selection with respect to both quiescent and star-forming galaxies. The numerous spectroscopic redshifts available in the EGS are used to train an artificial neural network to estimate photometric redshifts. The distribution of photometric redshift errors is Gaussian with standard deviation similar to 0.025(1 + z), and the fraction of redshift failures (>3 sigma errors) is about 3.5%. A new method of validation based on pair statistics confirms the estimate of standard deviation even for galaxies lacking spectroscopic redshifts. Basic galaxy properties measured include rest-frame U - B colors, B- and K-band absolute magnitudes, and stellar masses. We divide the sample into quiescent and star-forming galaxies according to their rest-frame U - B colors and 24-3.6 mu m flux density ratios and derive rest K-band luminosity functions and stellar mass functions for quiescent, star-forming, and all galaxies. The results show that massive, quiescent galaxies were in place by z approximate to 1, but lower mass galaxies generally ceased their star formation at later epochs.

Record 111 of 247

AGN host galaxies at redshift z ≈ 0.7: peculiar

or not?

Boehm, Asmus; Wisotzki, Lutz; Bell, Eric F.; Jahnke, Knud; Wolf, Christian; Bacon, David; Barden, Marco; Gray, Meghan E.; Hoeppe, Goetz; Jogee, Shardha; McIntosh, Dan H.; Peng, Chien Y.; Robaina, Adai R.; Balogh, Michael; Barazza, Fabio D.; Caldwell, John A. R.; Heymans, Catherine; Haeussler, Boris; Kampen, Eelco van; Lane, Kyle; Meisenheimer, Klaus; Sanchez, Sebastian F.; Taylor, Andy N.; Zheng, Xianzhong

Astronomy and Astrophysics

卷: 549; 期: 1; 页: 46-61

We perform a quantitative morphological comparison between the hosts of Active Galactic Nuclei (AGN) and quiescent galaxies at intermediate redshifts (z~0.7). The imaging data are taken from the large HST/ACS mosaics of the GEMS and STAGES surveys. Our main aim is to test whether nuclear activity at this cosmic epoch is triggered by major mergers. Using images of quiescent galaxies and stars, we create synthetic AGN images to investigate the impact of an optical nucleus on the morphological analysis of AGN hosts. Galaxy morphologies are parameterized using the asymmetry index A, concentration index


60

C, Gini coefficient G and M20 index. A sample of ~200 synthetic AGN is matched to 21 real AGN in terms of redshift, host brightness and host-to-nucleus ratio to ensure a reliable comparison between active and quiescent galaxies. The optical nuclei strongly affect the morphological parameters of the underlying host galaxy. Taking these effects into account, we find that the morphologies of the AGN hosts are clearly distinct from galaxies undergoing violent gravitational interactions. In fact, the host galaxies' distributions in morphological descriptor space are more similar to undisturbed galaxies than major mergers. Intermediate-luminosity (Lx < 10^44 erg/s) AGN hosts at z~0.7 show morphologies similar to the general population of massive galaxies with significant bulges at the same redshifts. If major mergers are the driver of nuclear activity at this epoch, the signatures of gravitational interactions fade rapidly before the optical AGN phase starts, making them undetectable on single-orbit HST images, at least with usual morphological descriptors. This could be investigated in future synthetic observations created from numerical simulations of galaxy-galaxy interactions.

Record 112 of 247

A DEEP SEARCH FOR MOLECULAR GAS IN TWO MASSIVE LYMAN BREAK GALAXIES AT z=3 AND 4: VANISHING CO-EMISSION DUE TO LOW METALLICITY?

Tan, Q.; Daddi, E.; Sargent, M.; Magdis, G.; Hodge, J.; Bethermin, M.; Bournaud, F.; Carilli, C.; Dannerbauer, H.; Dickinson, M.; Elbaz, D.; Gao, Y.; Morrison, G.; Owen, F.; Pannella, M.; Riechers, D.; Walter, F.


卷: 776; 期: 2; 页: L24-1-L24-6

We present deep IRAM Plateau de Bure Interferometer observations, searching for CO-emission toward two massive, non-lensed Lyman break galaxies at z = 3.216 and 4.058. With one low significance CO detection (3.5 sigma) and one sensitive upper limit, we find that the CO lines are greater than or similar to 3-4 times weaker than expected based on the relation between IR and CO luminosities followed by similarly massive galaxies at z = 0-2.5. This is consistent with a scenario in which these galaxies have low metallicity, causing an increased CO-to-H-2 conversion factor, i.e., weaker CO-emission for a given molecular (H-2) mass. The required

metallicities at z > 3 are lower than predicted by the fundamental metallicity relation at these redshifts, consistent with independent evidence. Unless our galaxies are atypical in this respect, detecting molecular gas in normal galaxies at z > 3 may thus remain challenging even with ALMA.

Record 113 of 247

A HERSCHEL SURVEY OF THE [N II] 205 mu m LINE IN LOCAL LUMINOUS INFRARED GALAXIES: THE [N II] 205 mu m EMISSION AS A STAR FORMATION RATE INDICATOR

Zhao, Yinghe; Lu, Nanyao; Xu, C. Kevin; Gao, Yu; Lord, S.; Howell, J.; Isaak, K. G.; Charmandaris, V.; Diaz-Santos, T.; Appleton, P.; Evans, A.; Iwasawa, K.; Leech, J.; Mazzarella, J.; Petric, A. O.; Sanders, D. B.; Schulz, B.; Surace, J.; van der Werf, P. P.


卷: 765; 期: 1; 页: L13-1-L13-6

We present, for the first time, a statistical study of [N II] 205 mu m line emission for a large sample of local luminous infrared galaxies using Herschel Spectral and Photometric Imaging Receiver Fourier Transform Spectrometer (SPIRE FTS) data. For our sample of galaxies, we investigate the correlation between the [N II] luminosity (L-[N II]) and the total infrared luminosity (L-IR), as well as the dependence of L-[N II]/L-IR ratio on L-IR, far-infrared colors (IRAS f(60)/f(100)), and the [O III] 88 mu m to [N II] luminosity ratio. We find that L-[N II] correlates almost linearly with L-IR for non-active galactic nucleus galaxies (all having L-IR < 10(12) L-circle dot) in our sample, which implies that L-[N II] can serve as a star formation rate tracer which is particularly useful for high-redshift galaxies that will be observed with forthcoming submillimeter spectroscopic facilities such as the Atacama Large Millimeter/submillimeter Array. Our analysis shows that the deviation from the mean L-[N II]-L-IR relation correlates with tracers of the ionization parameter, which suggests that the scatter in this relation is mainly due to the variations in the hardness, and/or ionization parameter, of the ambient galactic UV field among the sources in our sample.

Record 114 of 247

The Intrinsic Scatter Along The Main Sequence of Star-Forming Galaxies at z ~ 0.7

Guo, Kexin; Zheng, Xian Zhong; Fu, Hai


卷: 778; 期: 1; 页: 23-1-23-9


61

A sample of 12,614 star-forming galaxies (SFGs) with stellar mass >10(9.5) M-circle dot between 0.6 < z < 0.8 from COSMOS is selected to study the intrinsic scatter of the correlation between star formation rate (SFR) and stellar mass. We derive SFR from ultraviolet (UV) and infrared (IR) luminosities. A stacking technique is adopted to measure IR emission for galaxies undetected at 24 mu m. We confirm that the slope of the mass-SFR relation is close to unity. We examine the distributions of specific SFRs (SSFRs) in four equally spaced mass bins from 10(9.5) M-circle dot to 10(11.5) M-circle dot. Different models are used to constrain the scatter of SSFR for lower mass galaxies that are mostly undetected at 24 mu m. The SFR scatter is dominated by the scatter of UV luminosity and gradually that of IR luminosity at increasing stellar mass. We derive SSFR dispersions of 0.18, 0.21, 0.26, and 0.31 dex with a typical measurement uncertainty of less than or similar to 0.01 dex for the four mass bins. Interestingly, the scatter of the mass-SFR relation seems not constant in the sense that the scatter in SSFR is smaller for SFGs of stellar mass <10(10.5) M-circle dot. If confirmed, this suggests that the physical processes governing star formation become systematically less violent for less massive galaxies. The SSFR distribution for SFGs with intermediate mass 10(10)-10(10.)5 M-circle dot is characterized by a prominent excess of intense starbursts in comparison with other mass bins. We argue that this feature reflects that both violent (e.g., major/minor mergers) and quiescent processes are important in regulating star formation in this intermediate-mass regime.

Record 115 of 247

A Study on the Chemical Properties of Blue Compact Dwarf Galaxies

Zhao, Yinghe; Gao, Yu; Gu, Qiusheng


卷: 764; 期: 1; 页: 44-1-44-11

In this paper, we report our studies on the gaseous and chemical properties of a relatively large sample ( 53 members) of blue compact dwarf galaxies (BCDs). The results of correlations among the oxygen abundance, stellar mass, gas mass, baryonic mass, and gas fraction are present both for E-and I-type BCDs, which are classified according to Loose & Thuan and show elliptical and irregular outer haloes, respectively. These correlations of I-type BCDs show slopes similar to those of E-type ones. However, in general, E-type

BCDs are more gas-poor and metal-rich than I-type ones at a given baryonic mass. Based on these results, we suggest that E-type BCDs, at least a part of them, and I-type ones might be likely at different evolutionary phases and/or having different progenitors. Our investigation of the correlation between oxygen abundance and gas fraction shows that BCDs appear to have not evolved as isolated systems, but to have experienced some gas flows and/or mergers.

Record 116 of 247

Looking for molecular gas in a massive lyman break galaxy at z = 4.05

Tan, Qinghua; Daddi, Emanuele; Sargent, Mark; Hodge, Jackie; Gao, Yu

IAU Symposium

卷: 295; 期: 1; 页: 23

We present a search for CO emission in a massive lyman break galaxy at z~ 4.05.

Record 117 of 247

A Herschel Survey of the [NII] 205 micron Emission in Local Infrared Luminous Galaxies

Zhao, Yinghe; Lu, Nanyao; Xu, C. Kevin; Gao, Yu; GOALS FTS Team

Proceedings of the International Astronomical Union

卷: 8; 期: S292; 页: 256

The [N ii] line is a major coolant in ionized interstellar medium, and is expected to be a good star formation rate indicator. Here we present a statistical study of [N ii] line emission for a large sample of local luminous infrared galaxies (LIRGs) using Herschel SPIRE FTS data (Lu et al. 2012; Zhao et al. 2012, in preparation). For our sample of galaxies, the [N ii] to the total infrared luminosity

ratio (L [Nii]/L IR) varies from ？ 10-5 to ？ 10-4. We investigate the correlation between L [Nii] and L IR, as well as the dependence of L [Nii]/L IR on L IR, infrared colors (f60/f100) and the O III 88 μm to [N ii] luminosity ratio. We find that L [Nii] strongly, and almost linearly correlates with L IR for star-forming galaxies, namely log L IR = (4.23 ± 0.33) + (0.99 ± 0.05) log L [NII] (see Fig. 1). The scatter in this relation is mainly due to the variation of hardness, and/or high ionization parameter, of the background UV field.

Record 118 of 247


62

The Co-Evolution of Supermassive Black Holes and Galaxies: Observational Constraints

Zheng, Xianzhong

The intriguing life of massive galaxies, Proceedings IAU Symposium

期: 295; 页: 109-116

The connection between the growth of supermassive black holes (SMBHs) and the assembly of their host galaxies is termed `co-evolution'. Understanding co-evolution is one of the most fundamental issues in modern astrophysics. In this contribution, we review recent progress in addressing how the growth of SMBHs is linked to the properties of their host galaxies in the context of galaxy evolution, from the observational point of view. Although a coherent picture has not yet emerged, multiple pathways of co-evolution appear to be favored with a probable dependence on AGN luminosity and redshift.

Record 119 of 247

Muscle W49: A Multi-Scale Continuum And Line Exploration Of The Most Luminous Star Formation Region In The Milky Way. I. Data and the mass structure of the giant molecular cloud

Galvan-Madrid, R. ;Liu, H. B.; Zhang, Z-Y ; Pineda, J. E. ; Peng, T-C ; Zhang, Q.; Keto, E. R.; Ho, P. T. P. ; Rodriguez, L. F. ; Zapata, L. ; Peters, T. ;De Pree, C. G.


卷:779;期:2;页: 121(1-28)

The Multi-scale Continuum and Line Exploration of W49 is a comprehensive gas and dust survey of the giant molecular cloud (GMC) of W49A, the most luminous star-formation region in the Milky Way. The project covers, for the first time, the entire GMC at different scales and angular resolutions. In this paper, we present (1) an all-configuration Submillimeter Array mosaic in the 230 GHz (1.3 mm) band covering the central similar to 3' x 3' (similar to 10 pc, known as W49N), where most of the embedded massive stars reside and (2) Purple Mountain Observatory 14 m telescope observations in the 90 GHz band, covering the entire GMC with maps of up to similar to 35' x 35' in size, or similar to 113 pc. We also make use of archival data from the Very Large Array, JCMT-SCUBA, the IRAM 30 m telescope, and the Caltech Submillimeter Observatory BOLOCAM Galactic Plane Survey. We derive the basic physical parameters of the GMC at all scales.

Our main findings are as follows. (1) The W49 GMC is one of the most massive in the Galaxy, with a total mass M-gas similar to 1.1 x 10(6) M-circle dot within a radius of 60 pc. Within a radius of 6 pc, the total gas mass is M-gas similar to 2 x 10(5) M-circle dot. At these scales, only similar to 1% of the material is photoionized. The mass reservoir is sufficient to form several young massive clusters (YMCs) as massive as a globular cluster. (2) The mass of the GMC is distributed in a hierarchical network of filaments. At scales <10 pc, a triple, centrally condensed structure peaks toward the ring of HC H II regions in W49N. This structure extends to scales from similar to 10 to 100 pc through filaments that radially converge toward W49N and its less-prominent neighbor W49S. The W49A starburst most likely formed from global gravitational contraction with localized collapse in a "hub-filament" geometry. (3) Currently, feedback from the central YMCs (with a present mass M-cl greater than or similar to 5 x 10(4) M-circle dot) is still not enough to entirely disrupt the GMC, but further stellar mass growth could be enough to allow radiation pressure to clear the cloud and halt star formation. (4) The resulting stellar content will probably remain as a gravitationally bound massive star cluster or a small system of bound clusters.

Record 120 of 247

A Study on the Molecular Lines of CO Isotopes in the Star Forming Region AFGL 5157

MAO, Chun-hua; YANG, Ji; LU, Deng-rong


卷: 54; 期: 4; 页: 305-317

This paper presents a study of the dense molecular region AFGL 5157 over an area of

24’×24’（12 pc×12 pc）.We use the 13

CO（J=l-0）

and C18

0（J=1-0） observations to characterize the structure of the core.At the edge of the molecular cloud,the isotope abundance ratio X[(

13CO)/(C

180)]≈10,suggesting that the chemical

properties of AFGL 5157 cloud are similar to the giant molecular clouds.The virial masses of

13CO

and C18

0 are less than the mass of the molecular cloud core,so the molecular cloud core is gravitationally instable,and the C

180 molecular

Molecular Clouds and Star Formation


63

cloud core is easier to collapse.The column density distributions of the C

180 molecular cloud

core are,respectively,l.l×l023

×z-0.43

and 4.6×l0

25×z

-0.58 in the northeast direction and

southwest direction,where z is the distance from the center of the molecular cloud core.The high-velocity molecular outflow has been confirmed from our

12CO spectra,meanwhile the

mass loss rate of these sources has been got.Mass vs.velocity diagram for the outflow is fitted by a

power law distribution of m ∝ υ-1.8

.The star formation rate of the

13CO molecular cloud core is

23%.Maybe because of the effect of NGC 1985,AFGL 5157 is an active star forming region.

Record 121 of 247

Study on Description Methods of Mass Segregation of Star Clusters

ER, Xin-yue; JIANG, Zhi-bo; FU, Yan-ning

PROGRESS IN ASTRONOMY

卷: 31; 期: 2; 页: 202-212

Mass segregation means that the higher-mass stars are preferably found in the center of a cluster, whereas the lower-mass stars in the outer region. Studying mass segregation can help us to understand the dynamical evolution of clusters and constrain initial conditions of massive stars. There are a few dierent methods of probing mass segregation (or luminosity segregation when the masses of member stars are not available). These methods can be classified into two categories.

One is to investigate the dierence between stellar mass/luminosity functions (MF/LF) of two or more subregions of a cluster. In order to determine whether these functions are dierent or not, besides direct comparison, one may make use of some characteristic quantities, e.g. the ratio of mean stellar masses of two dierent subregions (<M>’). The other is to investigate the dierence between the stellar number density profiles (n0–r) of two or more sets of stars within dierent mass ranges. In order to determine whether these profiles are dierent or not, besides direct comparison, one may make use of some characteristic quantities, e.g. the ratio of half-number radii, lengths of the minimum

spanning tree (Λ ), and mean stellar mutual distances (R). Some tips of these methods are summarized as follows:

1) Since massive stars are usually scarce and MF is a piecewise defined function, describing mass segregation by the slope of MF should be careful.

2) <M>’ may be biased by the presence of a few massive stars.

3) The n0–r of one cluster may be not universal.

4) The ratio of half-number radii depends on the

cluster center, while it is not the case forΛand R.

There is no predominant method to describe mass segregation. In simulation, authors often study the evolution of mass segregation as a function of time, so <M>’ and R are preferred. In observation, authors often analyze only one cluster, so LF and n0–r seem to be more appropriate. In addition, if the velocities of member stars are available, one may consider the correlation between velocities and stellar masses as well.

Record 122 of 247

Mass segregation of embedded clusters in the Milky Way

Er, Xin-Yue; Jiang, Zhi-Bo; Fu, Yan-Ning


卷: 13; 期: 3; 页: 277-289

Embedded clusters are ideal laboratories for understanding the early phase of the dynamical evolution of clusters as well as massive star formation. An interesting observational phenomenon is that some of the embedded clusters show mass segregation, i.e., the most massive stars are preferentially found near the cluster center. We develop a new approach to describe mass segregation. Using this approach and the Two Micron All Sky Survey Point Source Catalog (2MASS PSC), we analyze 18 embedded clusters in the Galaxy. We find that 11 of them are mass-segregated and that the others are not mass-segregated. No inversely mass-segregated cluster is found.

Record 123 of 247

Hα emission objects in Circinus

Noroozi, S.; Haas, M.; Chen, Z.; Chini, R.

ASTRONOMISCHE NACHRICHTEN

卷: 334; 期: 3; 页: 282-287

We present a new survey for H alpha emission objects in the Circinus cloud complex and introduce an efficient photometric method for detecting H alpha emission via observations in a narrow-band filter. The observed flux is compared to a blackbody fit of the continuum. Our search strategy reveals 20 stars with strong H alpha emission (EW > 10 angstrom), eight of them being new detections. All H alpha stars display infrared


64

excess corroborating their youth. On the other hand, the region contains a number of infrared excess objects that do not show H alpha emission. Our results support the picture that accretion - as witnessed by H alpha emission - is a highly variable phenomenon. Therefore, H alpha surveys can only trace the temporarily active objects. In contrast, infrared excess is a more robust tracer that reveals most of the population of young stellar objects in a star forming region. Our analysis of the general stellar content of the region yields a reliable distance of 450 pc for the Circinus cloud. Moreover, we find a ratio of total-to-selective extinction of R-V = 2.8 suggesting that smaller-than-normal dust grains may be present.

Record 124 of 247

The thermal state of molecular clouds in the Galactic center: Evidence for non-photon-driven heating

Ao, Y.; Henkel, C.; Menten, K. M.; Requena-Torres, M. A.; Stanke, T.; Mauersberger, R.; Aalto, S.; Muehle, S.; Mangum, J.


卷: 550; 页: A135-1-A135-18

We used the Atacama Pathfinder Experiment (APEX) 12 m telescope to observe the J(KAKc) = 3(03) -> 2(02), 3(22) -> 2(21), and 3(21) -> 2(20) transitions of para-H2CO at 218 GHz simultaneously to determine kinetic temperatures of the dense gas in the central molecular zone (CMZ) of our Galaxy. The map extends over approximately 40' x 8' (similar to 100 x 20 pc(2)) along the Galactic plane with a linear resolution of 1.2 pc. The strongest of the three lines, the H2CO (3(03) -> 2(02)) transition, is found to be widespread, and its emission shows a spatial distribution similar to ammonia. The relative abundance of para-H2CO is 0.5 - 1.2 x 10(-9), which is consistent with results from lower frequency H2CO absorption lines. Derived gas kinetic temperatures for individual molecular clouds range from 50K to values in excess of 100 K. While a systematic trend toward (decreasing) kinetic temperature versus (increasing) angular distance from the Galactic center (GC) is not found, the clouds with highest temperature (T-kin > 100 K) are all located near the nucleus. For the molecular gas outside the dense clouds, the average kinetic temperature is 65 +/- 10 K. The high temperatures of molecular clouds on large scales in the GC region may be driven by turbulent

energy dissipation and / or cosmic-rays instead of photons. Such a non-photon-driven thermal state of the molecular gas provides an excellent template for the more distant vigorous starbursts found in ultraluminous infrared galaxies (ULIRGs).

Record 125 of 247

Young stars in epsilon Chamaleontis and their disks: disk evolution in sparse associations

Fang, M.; van Boekel, R.; Bouwman, J.; Henning, Th.; Lawson, W. A.; Sicilia-Aguilar, A.


卷: 549; 页: A15-1-A15-17

Context. The nearby young stellar association epsilon Cha has an estimated age of 3-5 Myr, making it an ideal laboratory to study the disk dissipation process and provide empirical constraints on the timescale of planet formation. Aims. We wish to complement existing optical and near-infrared data of the epsilon Cha association, which provide the stellar properties of its members, with mid-infrared data that probe the presence, geometry, and mineralogical composition of protoplanetary disks around individual stars. Methods. We combine the available literature data with our Spitzer/IRS spectroscopy and VLT/VISIR imaging data. We use proper motions to refine the membership of epsilon Cha. Masses and ages of individual stars are estimated by fitting model atmospheres to the optical and near-infrared photometry, followed by placement in the Hertzsprung-Russell diagram. The Spitzer/IRS spectra are analyzed using the two-layer temperature distribution spectral decomposition method. Results. Two stars previously identified as members, CXOU J120152.8 and 2MASS J12074597, have proper motions that are very different from those of the other stars. But other observations suggest that the two stars are still young and thus might still be related to epsilon Cha. HD104237C is the lowest mass member of epsilon Cha with an estimated mass of similar to 13-15 Jupiter masses. The very low mass stars USNO-B120144.7 and 2MASS J12005517 show globally depleted spectral energy distributions, pointing at strong dust settling. 2MASS J12014343 may have a disk with a very specific inclination, where the central star is effectively screened by the cold outer parts of a flared disk, but the 10 mu m radiation of the warm inner disk can still reach us. We find that the disks in sparse stellar associations are dissipated more slowly than those in denser


65

(cluster) environments. We detect C2H2 rovibrational band around 13.7 mu m on the IRS spectrum of USNO-B120144.7. We find strong signatures of grain growth and crystallization in all epsilon Cha members with 10 mu m features detected in their IRS spectra. We combine the dust properties derived in the epsilon Cha sample with those found using identical or similar methods in the MBM12, Coronet, eta Cha associations, and in the cores-to-disks legacy program. We find that disks around low-mass young stars show a negative radial gradient in the mass-averaged grain size and mass fraction of crystalline silicates. A positive correlation exists between the mass-averaged grain sizes of amorphous silicates and the accretion rates if the latter is above similar to 10(-9) M-circle dot yr(-1), possibly indicating that those disks are sufficiently turbulent to prevent grains of several microns in size to sink into the disk interior.

Record 126 of 247

Star-forming regions of the Aquila rift cloud complex I. NH3 tracers of dense molecular cores

Levshakov, S. A.; Henkel, C.; Reimers, D.; Wang, M.; Mao, R.; Wang, H.; Xu, Y.


卷: 553; 页: A58-1-A58-25

Aims. The physics of star formation is an important part of Galactic evolution. Most stars are formed in high-density environments (n > 10(4) cm(-3)) and emit lines of diverse molecular transitions. In the present part of our survey we search for ammonia emitters in the Aquila rift complex, which trace the densest regions of molecular clouds. Methods. From a CO survey carried out with the Delingha 14-m telescope we selected similar to 150 targets for observations in other molecular lines. Here we describe the mapping observations in the NH3(1, 1) and (2, 2) inversion lines of the first 49 sources performed with the Effelsberg 100-m telescope. Results. The NH3(1, 1) emission lines are detected in 12 and the (2, 2) in 7 sources. Among the newly discovered NH3 sources, our sample includes the following well-known clouds: the starless core L694-2, the Serpens cloud cluster B, the Serpens dark cloud L572, the filamentary dark cloud L673, the isolated protostellar source B335, and the complex star-forming region Serpens South. Angular sizes between 40 '' and 80 '' (similar to 0.04-0.08 pc) are observed for compact starless cores but can be as large as 9' (similar to 0.5 pc)

for filamentary dark clouds. The measured kinetic temperatures of the clouds lie between 9 K and 18 K. From NH3 excitation temperatures of 3-8 K we determine H-2 densities with typical values of similar to(0.4-4) x 10(4) cm(-3). The masses of the mapped cores range between similar to 0.05 and similar to 0.5 M-circle dot. The relative ammonia abundance X = [NH3]/[H-2] varies from 1 x 10(-7) to 5 x 10(-7) with the mean < X > = (2.7 +/- 0.6) x 10(-7) (estimated from spatially resolved cores assuming a filling factor of eta = 1). In two clouds, we observe kinematically split NH3 profiles separated by similar to 1 km s(-1). The splitting is most likely due to bipolar molecular outflows, for one of which we determine an acceleration of (V) over dot less than or similar to 0.03 km s(-1) yr(-1). A starless core with significant rotational energy is found to have a higher kinetic temperature than the other ones, which is probably caused by magnetic energy dissipation.

Record 127 of 247

OTS 44: Disk and accretion at the planetary border

Joergens, V.; Bonnefoy, M.; Liu, Y.; Bayo, A.; Wolf, S.; Chauvin, G.; Rojo, P.


卷: 558; 页: L7-1-L7-5

We discover that the very low-mass brown dwarf OTS 44 (M9.5, similar to 12 M-Jup) has significant accretion and a substantial disk, which demonstrates that the processes that accompany canonical star formation occur down to a central mass of a few Jupiter masses. We discover in VLT/SINFONI spectra that OTS 44 has strong, broad, and variable Pa beta emission that is evidence for active accretion at the planetary border. We also detect strong Ha emission of OTS 44 in a literature spectrum and determine an Ha EW of -141 angstrom, which indicates active accretion. Both the Pa beta and H alpha emission lines have broad profiles with wings extending to velocities of about +/- 200 km s(-1). We determine the mass accretion rate of OTS 44 based on H alpha to 7.6 x 10(-12) M-circle dot yr(-1). This result shows that OTS 44 has a relatively high mass-accretion rate considering its small central mass. This mass rate is nevertheless consistent with the general decreasing trend found for stars of several solar masses down to brown dwarfs. Furthermore, we determine the properties of the disk surrounding OTS 44 through radiative transfer modeling of flux measurement from the


66

optical to the far-IR (Herschel) by applying a Bayesian analysis. We find that OTS 44 has a highly flared disk (beta > 1.2) with a mass of 9.1(-5.5)(+1.7) x 10(-5) M-circle dot, i.e. similar to 0.1 M-Jup or 30 M-Earth. We show that the ratio of the disk-to-central-mass of about 10(-2) found for objects between 0.03 M-circle dot and 14 M-circle dot is also valid for OTS 44 at a mass of similar to 0.01 M-circle dot. Our observations are in line with an isolated star-like mode of the formation of brown dwarfs down to 0.01 M-circle dot.

Record 128 of 247

Refined physical properties and g', r', i', z', J, H, K transmission spectrum of WASP-23b from the ground

Nikolov, N.; Chen, G.; Fortney, J. J.; Mancini, L.; Southworth, J.; van Boekel, R.; Henning, Th.


卷: 553; 页: A26-1-A26-8

Context. Multi-band observations of planetary transits using the telescope defocus technique may yield high-quality light curves suitable for refining the physical properties of exoplanets even with small or medium size telescopes. Such observations can be used to construct a broad-band transmission spectrum of transiting planets and search for the presence of strong absorbers. Aims. We have thoroughly characterised the orbital ephemeris and physical properties of the transiting planet and host star in the WASP-23b system, constructed a broad-band transmission spectrum of WASP-23 b and performed a comparative analysis with theoretical models of hot Jupiters. Methods. We observed a complete transit of WASP-23 b in seven passbands simultaneously, using the GROND instrument on the MPG/ESO 2.2m telescope at La Silla Observatory and telescope defocussing. The optical data were taken in the Sloan g', r', i' and z' passbands. The resulting light curves are of high quality, with a root-mean-square scatter of the residual as low as 330 parts per million (ppm) in the z'-band, with a cadence of 90s. Near-infrared data were obtained in the JHK passbands. We performed a MCMC analysis of our photometry plus existing radial velocity data to refine measurements of the ephemeris and physical properties of the WASP-23 system. We constructed a broad-band transmission spectrum of WASP-23 b and compared it with a theoretical transmission spectrum of a hot Jupiter. Results.

We measured the central transit time with a precision similar to 8 s. From this and earlier observations we obtain an orbital period of P = 2.9444300 +/- 0.0000011 d. Our analysis also yielded a larger radius and mass for the planet (R-p = 1.067(-0.038)(+0.045) R-Jup and M-p = 0.917(-0.039)(+0.040) M-Jup) compared to previous estimates (R-p = 0.962(-0.056)(+0.047) R-Jup and M-p = 0.884(-0.094)(+0.088) M-Jup). The derived transmission spectrum is marginally flat, which is not surprising given the limited precision of the measurements for the planetary radius and the poor spectral resolution of the data.

Record 129 of 247

The link between magnetic fields and filamentary clouds: bimodal cloud orientations in the Gould Belt

Li, Hua-bai; Fang, Min; Henning, Thomas; Kainulainen, Jouni


卷: 436; 期: 4; 页: 3707-3719

The orientations of filamentary molecular clouds in the Gould Belt and their local intercloud media (ICM) magnetic fields are studied using near-infrared dust extinction maps and optical stellar polarimetry data. These filamentary clouds are a few-to-10 pc in length, and we find that their orientations tend to be either parallel or perpendicular to the mean field directions of the local ICM. This bimodal distribution is not found in cloud simulations with super-Alfvenic turbulence, in which the cloud orientations should be random. ICM magnetic fields that are dynamically important compared to inertial range turbulence and self-gravity can readily explain both field-filament configurations. Previous studies commonly recognize that strong magnetic fields can guide gravitational contraction and result in filaments perpendicular to them, but few discuss the fact that magnetic fields can also channel sub-Alfvenic turbulence to form filaments aligned with them. This strong-field scenario of cloud formation is also consistent with the constant field strength observed from ICM to clouds and is possible to explain the 'hub-filament' cloud structure and the density threshold of cloud gravitational contraction.

Record 130 of 247


67

Physical properties, transmission and emission spectra of the WASP-19 planetary system from multi-colour photometry

Mancini, L.; Ciceri, S.; Chen, G.; Tregloan-Reed, J.; Fortney, J. J.; Southworth, J.; Tan, T. G.; Burgdorf, M.; Novati, S. Calchi; Dominik, M.; Fang, X. -S.; Finet, F.; Gerner, T.; Hardis, S.; Hinse, T. C.; Jorgensen, U. G.; Liebig, C.; Nikolov, N.; Ricci, D.; Schaefer, S.; Schoenebeck, F.; Skottfelt, J.; Wertz, O.; Alsubai, K. A.; Bozza, V.; Browne, P.; Dodds, P.; Gu, S. -H.; Harpsoe, K.; Henning, Th.; Hundertmark, M.; Jessen-Hansen, J.; Kains, N.; Kerins, E.; Kjeldsen, H.; Lund, M. N.; Lundkvist, M.; Madhusudhan, N.; Mathiasen, M.; Penny, M. T.; Prof, S.; Rahvar, S.; Sahu, K.; Scarpetta, G.; Snodgrass, C.; Surdej, J.


卷: 436; 期: 1; 页: 2-18

We present new ground-based, multi-colour, broad-band photometric measurements of the physical parameters, transmission and emission spectra of the transiting extrasolar planet WASP-19b. The measurements are based on observations of eight transits and four occultations through a Gunn i filter using the 1.54-m Danish Telescope, 14 transits through an R-c filter at the Perth Exoplanet Survey Telescope (PEST) observatory and one transit observed simultaneously through four optical (Sloan g', r', i', z') and three near-infrared (J, H, K) filters, using the Gamma Ray Burst Optical and Near-Infrared Detector (GROND) instrument on the MPG/ESO 2.2-m telescope. The GROND optical light curves have a point-to-point scatter around the best-fitting model between 0.52 and 0.65 mmag rms. We use these new data to measure refined physical parameters for the system. We find the planet to be more bloated (R-b = 1.410 +/- 0.017R(Jup); M-b = 1.139 +/- 0.030M(Jup)) and the system to be twice as old as initially thought. We also used published and archived data sets to study the transit timings, which do not depart from a linear ephemeris. We detected an anomaly in the GROND transit light curve which is compatible with a spot on the photosphere of the parent star. The starspot position, size, spot contrast and temperature were established. Using our new and published measurements, we assembled the planet's transmission spectrum over the 370-2350 nm wavelength range and its emission spectrum over the 750-8000 nm range. By comparing these data to theoretical models we investigated the theoretically predicted variation

of the apparent radius of WASP-19b as a function of wavelength and studied the composition and thermal structure of its atmosphere. We conclude that: (i) there is no evidence for strong optical absorbers at low pressure, supporting the common idea that the planet's atmosphere lacks a dayside inversion; (ii) the temperature of the planet is not homogenized, because the high warming of its dayside causes the planet to be more efficient in re-radiating than redistributing energy to the night side; (iii) the planet seems to be outside of any current classification scheme.

Record 131 of 247

High-precision photometry by telescope defocusing – V. WASP-15 and WASP-16

Southworth, John; Mancini, L.; Browne, P.; Burgdorf, M.; Novati, S. Calchi; Dominik, M.; Gerner, T.; Hinse, T. C.; Jorgensen, U. G.; Kains, N.; Ricci, D.; Schaefer, S.; Schoenebeck, F.; Tregloan-Reed, J.; Alsubai, K. A.; Bozza, V.; Chen, G.; Dodds, P.; Dreizler, S.; Fang, X. -S.; Finet, F.; Gu, S. -H.; Hardis, S.; Harpsoe, K.; Henning, Th; Hundertmark, M.; Jessen-Hansen, J.; Kerins, E.; Kjeldsen, H.; Liebig, C.; Lund, M. N.; Lundkvist, M.; Mathiasen, M.; Nikolov, N.; Penny, M. T.; Proft, S.; Rahvar, S.; Sahu, K.; Scarpetta, G.; Skottfelt, J.; Snodgrass, C.; Surdej, J.; Wertz, O.


卷: 434; 期: 3; 页: 1300-1308

We present new photometric observations of WASP-15 and WASP-16, two transiting extrasolar planetary systems with measured orbital obliquities but without photometric follow-up since their discovery papers. Our new data for WASP-15 comprise observations of one transit simultaneously in four optical passbands using GROND on the MPG/European Southern Observatory (ESO) 2.2 m telescope, plus coverage of half a transit from DFOSC on the Danish 1.54 m telescope, both at ESO La Silla. For WASP-16 we present observations of four complete transits, all from the Danish telescope. We use these new data to refine the measured physical properties and orbital ephemerides of the two systems. Whilst our results are close to the originally determined values for WASP-15, we find that the star and planet in the WASP-16 system are both larger and less massive than previously thought.

Record 132 of 247


68

PHOTOMETRY OF VARIABLE STARS FROM DOME A, ANTARCTICA: RESULTS FROM THE 2010 OBSERVING SEASON

Wang, Lingzhi; Macri, Lucas M.; Wang, Lifan; Ashley, Michael C. B.; Cui, Xiangqun; Peng, Long-Long; Gong, Xuefei; Lawrence, Jon S.; Liu, Qiang; Daniel Luong-Van; Pennypacker, Carl R.; Shang, Zhaohui; Storey, John W. V.; Yang, Huigen; Yang, Ji; Yuan, Xiangyan; York, Donald G.; Zhou, Xu; Zhu, Zhenxi; Zhu, Zonghong


卷: 146; 期: 6; 页: 139-1-139-10

We present results from a season of observations with the Chinese Small Telescope ARray, obtained over 183 days of the 2010 Antarctic winter. We carried out high-cadence time-series aperture photometry of 9125 stars with i less than or similar to 15.3 mag located in a 23 deg(2) region centered on the south celestial pole. We identified 188 variable stars, including 67 new objects relative to our 2008 observations, thanks to broader synoptic coverage, a deeper magnitude limit, and a larger field of view. We used the photometric data set to derive site statistics from Dome A. Based on two years of observations, we find that extinction due to clouds at this site is less than 0.1 and 0.4 mag during 45% and 75% of the dark time, respectively.

Record 133 of 247

Ground-based Detections of Thermal Emission from the Dense Hot Jupiter WASP-43b in the H and Ks Bands

Wang, W.; van Boekel, R.; Madhusudhan, N.; Chen, G.; Zhao, G.; Henning, Th.


卷: 770; 期: 1; 页: 70-1-70-8

We report new detections of thermal emission from the transiting hot Jupiter WASP-43b in the H and K-s bands as observed at secondary eclipses. The observations were made with the WIRCam instrument on the Canada-France-Hawaii Telescope. We obtained a secondary eclipse depth of 0.103(-0.017)(+0.017)% and 0.194(-0.029)(+0.029)% in the H and K-s bands, respectively. The K-s-band depth is consistent with the previous measurement in the narrow band centered at 2.09 mu m by Gillon et al. Our eclipse depths in both bands are consistent with a blackbody spectrum with a temperature of similar to 1850 K, slightly higher than the dayside equilibrium temperature without day-night energy redistribution. Based on theoretical

models of the dayside atmosphere of WASP-43b, our data constrain the day-night energy redistribution in the planet to be less than or similar to 15%-25%, depending on the metal content in the atmosphere. Combined with energy balance arguments, our data suggest that a strong temperature inversion is unlikely in the dayside atmosphere of WASP-43b. However, a weak inversion cannot be strictly ruled out at the current time. Future observations are required to place detailed constraints on the chemical composition of the atmosphere.

Record 134 of 247

AFGL 5157 NH3: a new stellar cluster in the forming process

Jiang, Zhi-Bo; Chen, Zhi-Wei; Wang, Yuan; Yang, Ji; Huang, Jia-Sheng; Zhang, Qi-Zhou; Fazio, Giovani


卷: 13; 期: 6; 页: 695-704

We present the analysis of Spitzer/IRAC and near infrared imaging observation of AFGL 5157, an active star forming region. In the IRAC images, this region shows strong emissions of polycyclic aromatic hydrocarbons in channel 4 and emissions of H-2 in channel 2. Many of the H-2 features are aligned to form jet-like structures. Three bipolar jets in the NH3 core region and a couple of jets northwest of the core have been identified. We identify the possible driving agents of the bipolar jets and show them to be very young. An embedded cluster has been detected in the NH3 core; many members in the cluster have spectral energy distributions that increase from JHK bands toward longer wavelengths, indicative of their early evolutionary stages. Millimeter and submillimeter continuum emissions in the NH3 core and the northwest subregion are found to coincide spatially with these presumable Class 0/I sources. The existence of H-2 bipolar jets and very young stellar objects suggests that star formation is continuing at the present epoch in these subregions. Combining information from previous studies, we propose a sequential star formation scenario in the whole AFGL 5157 region.

Record 135 of 247

CO observations of the Galactic bubble N4

Li, Jun-Yu; Jiang, Zhi-Bo; Liu, Yao; Wang, Yuan


卷: 13; 期: 8; 页: 921-934

We present a study of the Galactic bubble N4


69

using the 13.7 m millimeter-wave telescope, which is managed by Purple Mountain Observatory at Qinghai Station. N4 is one of the science demonstration regions where simultaneous observations of (CO)-C-12 (J = 1 - 0), (CO)-C-13 (J = 1 - 0) and (CO)-O-18 (J = 1 - 0) line emission towards N4 were carried out under the project Milky Way Imaging Scroll Painting (MWISP). We analyze the spectral profile and the distribution of the molecular gas. Morphologically, the CO emissions correlate well with Spitzer IRAC 8.0 mu m emission. The channel map and velocity-position diagram show that N4 is more likely to be an inclined expanding ring rather than a spherical bubble. We calculated the physical parameters of N4 including mass, size, column density and optical depth. Some massive star candidates were discovered in the region of N4 using the (J, J - H) color-magnitude diagram. We found a candidate for the energy source driving the expansion of N4, a massive star with a mass of similar to 15 M-circle dot and an age of similar to 1 Myr. There is the signature of infall motion in N4, which can be a good candidate for the infall area. Combining millimeter and infrared data, we suggest that triggered star formation can exist in N4.

Record 136 of 247

A comparison of approaches in fitting continuum SEDs

Liu, Yao; Madlener, David; Wolf, Sebastian; Wang, Hong-Chi


卷: 13; 期: 4; 页: 420-434

We present a detailed comparison of two approaches, the use of a pre-calculated database and simulated annealing (SA), for fitting the continuum spectral energy distribution (SED) of astrophysical objects whose appearance is dominated by surrounding dust. While pre-calculated databases are commonly used to model SED data, only a few studies to date employed SA due to its unclear accuracy and convergence time for this specific problem. From a methodological point of view, different approaches lead to different fitting quality, demand on computational resources and calculation time. We compare the fitting quality and computational costs of these two approaches for the task of SED fitting to provide a guide to the practitioner to find a compromise between desired accuracy and available resources. To

reduce uncertainties inherent to real datasets, we introduce a reference model resembling a typical circumstellar system with 10 free parameters. We derive the SED of the reference model with our code MC3D at 78 logarithmically distributed wavelengths in the range [0.3 mu m, 1.3 mm] and use this setup to simulate SEDs for the database and SA. Our result directly demonstrates the applicability of SA in the field of SED modeling, since the algorithm regularly finds better solutions to the optimization problem than a pre-calculated database. As both methods have advantages and shortcomings, a hybrid approach is preferable. While the database provides an approximate fit and overall probability distributions for all parameters deduced using Bayesian analysis, SA can be used to improve upon the results returned by the model grid.

Record 137 of 247

Radiative transfer modeling of three T Tauri stars: selecting candidates for studying circumstellar disk evolution

Liu, Yao; Wang, Hong-Chi; Wolf, Sebastian; Madlener, David


卷: 13; 期: 7; 页: 841-848

We present modeling work on three young stellar objects that are promising targets for future high-resolution observations to investigate circumstellar disk evolution. The currently available data comprise the spectral energy distribution from optical to millimeter wavelengths which allow constraining the structure of the circumstellar disk using self-consistent radiative transfer models. The results suggest that the assumption of well-mixed dust and gas leads to overestimation of flux in the far-infrared. Observational and theoretical arguments suggest that an overall decrease in far-infrared excess can be explained by dust settling towards the midplane. A new disk model is hence employed to take the effect of dust sedimentation into account. The extended model satisfactorily reproduces all existing observations. The three targets studied here therefore deserve follow-up observations to reveal the evolutionary state of their protoplanetary disks.

Record 138 of 247


70

Conceptual design studies of the 5m terahertz antenna for Dome A, Antarctica

Yang, Ji; Zuo, Ying-Xi; Lou, Zheng; Cheng, Jing-Quan; Zhang, Qi-Zhou; Shi, Sheng-Cai; Huang, Jia-Sheng; Yao, Qi-Jun; Wang, Zhong


卷: 13; 期: 12; 页: 1493-1508

As the highest, coldest and driest place in Antarctica, Dome A provides exceptionally good observing conditions for ground-based observations over terahertz wavebands. The 5m Dome A Terahertz Explorer (DATE5) has been proposed to explore new terahertz windows, primarily over wavelengths between 350 and 200 mu m. DATE5 will be an open-air, fully-steerable telescope that can function by unmanned operation with remote control. The telescope will be able to endure the harsh polar environment, including high altitude, very low temperature and very low air pressure. The unique specifications, including high accuracies for surface shape and pointing and fully automatic year-around remote operation, along with a stringent limit on the periods of on-site assembly, testing and maintenance, bring a number of challenges to the design, construction, assembly and operation of this telescope. This paper introduces general concepts related to the design of the DATE5 antenna. Beginning from an overview of the environmental and operational limitations, the design specifications and requirements of the DATE5 antenna are listed. From these, major aspects on the conceptual design studies, including the antenna optics, the backup structure, the panels, the subreflector, the mounting and the antenna base structure, are explained. Some critical issues of performance are justified through analyses that use computational fluid dynamics, thermal analysis and de-icing studies, and the proposed approaches for test operation and on-site assembly. Based on these studies, we conclude that the specifications of the DATE5 antenna can generally be met by using enhanced technological approaches.

Record 139 of 247

CEN 34-high-mass YSO in M 17 or background post-AGB star?

Chen, Zhiwei; Nurnberger, Dieter E.A.; Chini, Rolf; Liu, Yao; Fang, Min; Jiang, Zhibo

Astronomy and Astrophysics

卷: 557; 期: 1; 页: A51-A59

We investigate the proposed high-mass young stellar object (YSO) candidate CEN 34, thought to be associated with the star-forming region M 17. Its optical to near-infrared (550-2500 nm) spectrum reveals several photospheric absorption features, such as H, the Ca ii triplet, and the CO bandhead, but lacks emission lines. The spectral features in the range 8375-8770 A are used to constrain an effective temperature Teff = 5250 250 K (early-/mid-G) and a log g = 2.0 0.3 (supergiant). The spectral energy distribution (SED) displays a faint infrared excess that resembles that of a high-mass YSO or an evolved star of intermediate mass. Moreover, the observed temperature and surface gravity are identical for high-mass YSOs and evolved stars. The radial velocity of CEN 34 relative to the local standard of rest (VLSR) as obtained from various photospheric lines is of the order of-60 km s-1 and thus distinct from the +25 km s-1 found for several OB stars in the cluster and for the associated molecular cloud. The SED modeling yields 10-4 MS of circumstellar material, which contributes only a tiny fraction to the total visual extinction (11 mag). The distance of CEN 34 is between 2.0 kpc and 4.5 kpc. In the case of a YSO, a dynamical ejection process is proposed to explain the VLSR difference between CEN 34 and M 17. Additionally, to match the temperature and luminosity, we speculate that CEN 34 had accumulated the bulk of its mass with an accretion rate 4 10-3MS/yr over a very short time span (103 yrs), and it is currently undergoing a phase of gravitational contraction without any further mass gain. However, all the aforementioned characteristics of CEN 34 are compatible with an evolved star of 5-7 MS and an age of 50-100 Myr, so it is most likely a background post-AGB star with a distance between 2.0 kpc and 4.5 kpc. We consider the latter classification as the more likely interpretation. Further discrimination of the two possible scenarios should come from the stricter confinement of CEN 34's distance. 2013 ESO.

Record 140 of 247

Proper motions of molecular hydrogen outflows in the rho Ophiuchi molecular cloud

Zhang, M.; Brandner, W.; Wang, H.; Gennaro, M.; Bik, A.; Henning, Th; Gredel, R.; Smith, M.; Stanke, Th


卷: 553; 页: A41-1-A41-37

Context. Proper motion measurements provide


71

unique and powerful means to identify the driving sources of mass outflows, which are of particular importance in regions with complex star formation activity and deeply embedded protostars. They also provide the necessary kinematic information to study the dynamics of mass outflows, the interaction between outflows and the ambient medium, and the evolution of outflows with the age of the driving sources. Aims. We aim to take a census of molecular hydrogen emission line objects (MHOs) in the rho Ophiuchi molecular cloud and to make the first systematic proper motion measurements of these objects in this region. The driving sources are identified based on the measured proper motions, and the outflow properties are characterized. The relationship between outflow properties and the evolutionary stages of the driving sources are also investigated. Methods. Deep H-2 near-infrared imaging is performed to search for molecular hydrogen emission line objects. Multi-epoch data are used to derive the proper motions of the features of these objects, and the lengths and opening angles of the molecular hydrogen outflows. Results. Our imaging covers an area of similar to 0.11 deg(2) toward the L1688 core in the rho Ophiuchi molecular cloud. In total, six new MHOs are discovered, 32 previously known MHOs are detected, and the proper motions for 86 features of the MHOs are measured. The proper motions lie in the range of 14 to 247 mas/yr, corresponding to transversal velocities of 8 to 140 km s(-1) with a median velocity of about 35 km s(-1). Based on morphology and proper motion measurements, 27 MHOs are ascribed to 21 driving sources. The molecular hydrogen outflows have a median length of similar to 0.04 pc and random orientations. We find no obvious correlation between H-2 jet length, jet opening angle, and the evolutionary stage of the driving sources as defined by their spectral indices. We find that the fraction of protostars (23%) that drive molecular hydrogen outflows is similar to the one for Class II sources (15%). For most molecular hydrogen outflows, no obvious velocity variation along the outflow has been found. Conclusions. In Ophiuchus the frequency of occurrence of molecular hydrogen outflows has no strong dependency on the evolutionary stage of the driving source during the evolution from the protostellar stage to the classical T Tauri stage.

Record 141 of 247

SMA OBSERVATIONS OF CLASS 0 PROTOSTARS: A HIGH ANGULAR RESOLUTION SURVEY OF PROTOSTELLAR BINARY SYSTEMS

Chen, Xuepeng; Arce, Hector G.; Zhang, Qizhou; Bourke, Tyler L.; Launhardt, Ralf; Jorgensen, Jes K.; Lee, Chin-Fei; Foster, Jonathan B.; Dunham, Michael M.; Pineda, Jaime E.; Henning, Thomas


卷: 768; 期: 2; 页: 110-1-110-31

We present high angular resolution 1.3 mm and 850 mu m dust continuum data obtained with the Submillimeter Array toward 33 Class 0 protostars in nearby clouds (distance < 500 pc), which represents so far the largest survey toward protostellar binary/multiple systems. The median angular resolution in the survey is 2 ''.5, while the median linear resolution is approximately 600 AU. Compact dust continuum emission is observed from all sources in the sample. Twenty-one sources in the sample show signatures of binarity/multiplicity, with separations ranging from 50 AU to 5000 AU. The numbers of singles, binaries, triples, and quadruples in the sample are 12, 14, 5, and 2, respectively. The derived multiplicity frequency (MF) and companion star fraction (CSF) for Class 0 protostars are 0.64 +/- 0.08 and 0.91 +/- 0.05, respectively, with no correction for completeness. The derived MF and CSF in this survey are approximately two times higher than the values found in the binary surveys toward Class I young stellar objects, and approximately three (for MF) and four (for CSF) times larger than the values found among main-sequence stars, with a similar range of separations. Furthermore, the observed fraction of high-order multiple systems to binary systems in Class 0 protostars (0.50 +/- 0.09) is also larger than the fractions found in Class I young stellar objects (0.31 +/- 0.07) and main-sequence stars (<= 0.2). These results suggest that binary properties evolve as protostars evolve, as predicted by numerical simulations. The distribution of separations for Class 0 protostellar binary/multiple systems shows a general trend in which CSF increases with decreasing companion separation. We find that 67% +/- 8% of the protobinary systems have circumstellar mass ratios below 0.5, implying that unequal-mass systems are preferred in the process of binary star formation. We suggest an empirical sequential fragmentation picture for binary star formation, based on this work and existing lower resolution single-dish observations.


72

Record 142 of 247

YOUNG STELLAR OBJECTS IN LYNDS 1641: DISKS, ACCRETION, AND STAR FORMATION HISTORY

Fang, Min; Kim, Jinyoung Serena; van Boekel, Roy; Sicilia-Aguilar, Aurora; Henning, Thomas; Flaherty, Kevin

ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES

卷: 207; 期: 1; 页: 5-1-5-39

We investigate the young stellar objects (YSOs) in the Lynds 1641 (L1641) cloud using multi-wavelength data including Spitzer, WISE, the Two Micron All Sky Survey, and XMM covering similar to 1390 YSOs across a range of evolutionary stages. In addition, we targeted a sub-sample of YSOs for optical spectroscopy with the MMT/Hectospec and the MMT/Hectochelle. We use these data, along with archival photometric data, to derive spectral types, extinction values, masses, ages, and accretion rates. We obtain a disk fraction of similar to 50% in L1641. The disk frequency is almost constant as a function of stellar mass with a slight peak at log(M-*/M-circle dot) approximate to -0.25. The analysis of multi-epoch spectroscopic data indicates that the accretion variability of YSOs cannot explain the two orders of magnitude of scatter for YSOs with similar masses. Forty-six new transition disk (TD) objects are confirmed in this work, and we find that the fraction of accreting TDs is lower than for optically thick disks (40%-45% versus 77%-79%, respectively). We confirm our previous result that the accreting TDs have a median accretion rate similar to normal optically thick disks. We confirm that two star formation modes (isolated versus clustered) exist in L1641. We find that the diskless YSOs are statistically older than the YSOs with optically thick disks and the TD objects have a median age that is intermediate between those of the other two populations. We tentatively study the star formation history in L1641 based on the age distribution and find that star formation started to be active 2-3 Myr ago.

Record 143 of 247

Unveiling the Physical Properties and Kinematics of Molecular Gas in the Antennae Galaxies with the SMA

Ueda, J.; Iono, D.; Petitpas, G.; Yun, M. S.; Ho, P. T. P.; Kawabe, R.; Mao, R.-Q.; Martín, S.; Matsushita, S.; Peck, A. B.; Tamura, Y.; Wang, J.; Wang, Z.; Wilson, C. D.; Zhang, Q.

ASP Conference Proceedings

卷: 477; 期: 1; 页: 311-312

We present a ~1'' (100 pc) resolution 12CO (3-2) map of the nearby intermediate-stage interacting galaxy pair NGC 4038/9 (the Antennae galaxies) obtained with the Submillimeter Array. We find that half the CO (3-2) emission originates in the overlap region where most of the tidally induced star formation had been previously found in shorter wavelength images, with the rest being centered on each of the nuclei. The gross distribution is consistent with lower resolution single-dish images, but we show for the first time the detailed distribution of the warm and dense molecular gas across this galaxy pair at resolutions comparable to the size of a typical giant molecular complex. While we find that 58% (33/57) of the spatially resolved Giant Molecular Associations (a few × 100 pc) are located in the overlap region, only ≤30% spatially coincides with the optically detected star clusters, suggesting that the bulk of the CO (3-2) emission traces the regions with very recent or near future star formation activity. The spatial distribution of the CO (3-2)/CO (1-0) integrated brightness temperature ratios mainly ranges between 0.3 and 0.6, which suggests that on average the CO (3-2) line in the Antennae is not completely thermalized and similar to the average values of nearby spirals. A higher ratio is seen in both nuclei and the southern complexes in the overlap region. A higher radiation field associated with intense star formation can account for the nucleus of NGC 4038 and the overlap region, but the nuclear region of NGC 4039 shows relatively little star formation or active galactic nucleus activity and cannot be easily explained. We show kinematical evidence that the high line ratio in NGC 4039 is possibly caused by gas inflow into the counter-rotating central disk.

Record 144 of 247

Molecular Gas Around the Infrared Dust Bubbles

Gong, Yan; Mao, Ruiqing; Fang, Min; Sun, Jixian; Lu, Dengrong


卷: 8; 期: S292; 页: 43

We have conducted a mapping survey toward a sample of 17 infrared dust bubbles in three 3 mm waveband CO isotopic lines simultaneously. Such bubbles are candidates to search for triggered massive star formation. We present the data and report preliminary results.


73

Record 145 of 247

Triggered Star Formation at the End of the Galactic Bar?

Gong, Yan; Mao, Ruiqing; Henkel, Christian; Urquhart, James; Wang, Yuan; Zhang, Zhiyu; Wyrowski, Friedrich

Protostars and Planets VI

期: VI

The interstellar bubble N36 created by an HII region and surrounded by a swept-up layer is an exceptional target to study triggered massive star formation. Combining infrared and radio data, N36 turns out to be a vigorous star forming region at a location where the Norma Galactic arm meets the Galactic bar. This makes it possible to investigate in spatial detail conditions of a molecular cloud affected by the presence of a large scale bar.

Record 146 of 247

Gradients Of Stellar Population Properties And Evolution Clues In A Nearby Galaxy M101

Lin, Lin ; Zou, Hu ; Kong, Xu ; Lin, Xuanbin ;Mao, Yewei ;Cheng, Fuzhen ; Jiang, Zhaoji; Zhou, Xu


卷:769;期:2;页: 127(1-13)

Multiband photometric images from ultraviolet and optical to infrared are collected to derive spatially resolved properties of the nearby Scd-type galaxy M101. With evolutionary stellar population synthesis models, two-dimensional distributions and radial profiles of age, metallicity, dust attenuation, and star formation timescale in the form of the Sandage star formation history are obtained. When fitting with the models, we use the IRX-A(FUV) relation, found to depend on a second parameter of birth rate b (ratio of present-and past-averaged star formation rates), to constrain the dust attenuation. There are obvious parameter gradients in the disk of M101, which supports the theory of an "inside-out" disk growth scenario. Two distinct disk regions with different gradients of age and color are discovered, similar to another late-type galaxy, NGC 628. The metallicity gradient of the stellar content is flatter than that of HII regions. The stellar disk is optically thicker inside than outside and the global dust attenuation of this galaxy is lower compared with galaxies of similar and earlier morphological type. We note that a variational star formation timescale describes the real star formation history

of a galaxy. The timescale increases steadily from the center to the outskirt. We also confirm that the bulge in this galaxy is a disk-like pseudobulge, whose evolution is likely to be induced by some secular processes of the small bar which is relatively young, metal-rich, and contains much dust.

Record 147 of 247

Initial Considerations of the 5 Meter Dome A Terahertz Explorer (DATE5) for Antarctica

Yang, Ji ; Lou, Zheng ; Zuo, Yingxi;Cheng, Jingquan

International Symposium on Antennas and Propagation (ISAP)

卷:1;页: 21-24

Terahertz radiation comes from cold objects in universe. It provides important information of star and galaxy formation. Within these bands, thousands of molecular lines are located, which may reveal important processes in cosmology. In Antarctica, the Dome A area has the best observing windows in the terahertz waveband. In this paper, a 5 meters Dome A Terahertz Explorer (DATE5) telescope concept is provided, which is a fully steerable telescope, working under the harsh Dome A polar environments. It requires a higher surface and pointing accuracies. This paper also discusses major aspects to be taken into consideration in its initial conceptual study.

Record 148 of 247

Design of Bandpass Filters Using Three Parallel Coupled-Lines with Open Stub Resonator

Tian, Ge; Yang, Jinping; Wu, Wen

CHINESE JOURNAL OF ELECTRONICS

卷: 22; 期:1; 页: 192-194

Bandpass filter with equal-ripple response in the passband and four transmission zeros in the stopband is synthesized in this letter. Equivalent circuit model is proposed. Based on even- and odd-mode theory, design formulas are derived to provide relationship between filtering

Laboratory for Millimeter &

Sub-Millimeter Wave


74

characteristics (center frequency, bandwidth, and transmission zeros) and circuit parameters for the filter. To verify the design concept, a bandpass filter with a fractional bandwidth of 26.7% (ripple level 0.01dB) at the center frequency of 3.9 GHz is designed and fabricated. The measured insertion loss is less than 0.6 dB, and return loss is higher than 19.4 dB in the passband. The stopband extends to 10.4 GHz with the rejection level of 20 dB. Measured results show good agreement with simulations.

Record 149 of 247

Development of a Dual Polarization SIS Mixer With a Planar Orthomode Transducer at 350 GHz

Liu, Kuan-Yu; Wang, Ming-Jye; Li, Chao-Te; Chen, Tse-Jun; Shi, Sheng-Cai

IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY

卷:23; 期: 3; 页: 1400705-1-1400705-5

A multipixel array equipped with dual-polarization superconductor-insulator-superconductor junction mixers at approximately 350 GHz is considered to improve the efficiency and survey speed of a telescope. This study develops a compact mixer with a planar orthomode transducer as a key component. Signals coming from a circular waveguide are separated into two polarizations via orthogonal waveguide probes, and then transmitted to the junctions through the tuning circuit. To suppress resonance, metallic blocks confine the RF signals within the circular waveguide, and a 2-mu m-thick silicon nitride membrane, on which all devices were implemented, was suspended across the circular waveguide. The orthomode transducer, simulated with a three-dimensional electromagnetic simulator, has a cross-polarization of less than -20 dB between 306 and 367 GHz. The IF circuit consists of a low pass filter, coplanar waveguides, and a transition to coaxial. The return loss of the IF circuit is less than -20 dB up to 16 GHz from both simulations and measurements. The superconductor-insulator-superconductor junction mixers have been fabricated with quality factor (R-sg/R-n) of 8 and the double-side-band receiver noise temperature T-rx is approximately 120 K between 320 and 360 GHz.

Record 150 of 247

The influence of CeO2 nano-dots decoration on substrates on flux pinning strength in Tl2Ba2CaCu2O8 thin films

Ji, Lu; Gao, Xiaoxin; Ge, Deyong; Xie, Wei; Wang, Pei; Zhao, Xinjie; Wang, Zheng; He, Ming; Zhang, Xu; Li, Wei; Song, Feng; Yan, Shaolin


卷: 23; 期: 3; 页: 8001505-1-8001505-5

Nano-sized CeO2 dots were deposited on (001) LaAlO3 substrate by rf magnetron sputtering. After the processing of the artificial decoration defects on the substrate, 100-nm, 150-nm, 200-nm, and 400-nm-thick Tl2Ba2CaCu2O8 (Tl-2212) thin films were grown on it, using dc magnetron sputtering and post annealing process. AFM images showed that the CeO2 nanodots were distributed well on the substrate surface with 70 nm in diameter and 5 nm in height, and the density of nano-dots was 25 +/- 3 dots/mu m(2). SEM images were used to observe the variations on film surface. Transport critical current density J(c) was measured both on Tl-2212 film with nano-dots decorated substrate and untreated single crystal LaAlO3 substrate. From the results, J(c) values of Tl-2212 films with nano-dots decorated substrate were lifted significantly, and the pinning strength was improved on Tl-2212 films by nanostructure defects induced from nano-dots.

Record 151 of 247

Beam and phase distributions of a terahertz quantum cascade wire laser

Cui, M.; Hovenier, J. N.; Ren, Y.; Vercruyssen, N.; Gao, J. R.; Kao, T. Y.; Hu, Q.; Reno, J. L.

APPLIED PHYSICS LETTERS

卷: 102; 期: 11; 页: 111113-1-111113-5

We report on both measurements and simulations of the beam profile and wavefront of a single-mode, 3.5 THz quantum cascade wire laser, incorporating a lateral corrugated metal-metal waveguide, 3rd-order distributed feedback grating. The intrinsic wavefront was measured by using a Hartmann wavefront sensor (HWS) without any optical components between the laser and HWS. Both beam profile and wavefront were simulated using an antenna array model, but taking the non-uniform electric field distribution along the waveguide into account. The results show that the non-uniform distribution along the wire laser


75

plays a crucial role in realizing a nearly single-lobed narrow beam. The measured wavefront is spherical and agrees well with the simulation.

Record 152 of 247

Hot electron bolometer heterodyne receiver with a 4.7-THz quantum cascade laser as a local oscillator

Kloosterman, J. L.; Hayton, D. J.; Ren, Y.; Kao, T. Y.; Hovenier, J. N.; Gao, J. R.; Klapwijk, T. M.; Hu, Q.; Walker, C. K.; Reno, J. L.

APPLIED PHYSICS LETTERS

卷: 102; 期: 1; 页: 11123-1-11123-4

We report on a heterodyne receiver designed to observe the astrophysically important neutral atomic oxygen [OI] line at 4.7448 THz. The local oscillator is a third-order distributed feedback quantum cascade laser operating in continuous wave mode at 4.741 THz. A quasi-optical, superconducting NbN hot electron bolometer is used as the mixer. We recorded a double sideband receiver noise temperature (T-rec(DSB)) of 815 K, which is similar to 7 times the quantum noise limit (hv/2k(B)) and an Allan variance time of 15 s at an effective noise fluctuation bandwidth of 18 MHz. Heterodyne performance was confirmed by measuring a methanol line spectrum.

Record 153 of 247

Characterization of the IF Bandwidth of an All-NbN Superconductor-Insulator-Superconductor Mixer

Liu, D.; Li, J.; Wang, Z.; Yao, M.; Hu, J.; Shi, S. C.


卷: 23; 期:3; 页: 1400504-1-1400504-4

Large intermediate-frequency (IF) bandwidth is of particular interest for heterodyne mixers, especially for those at THz frequencies. NbN superconductor-insulator-superconductor (SIS) junctions, with a gap frequency twice that of Nb, can be applied to mixers beyond 1 THz. The IF bandwidth of NbN SIS mixers, however, is yet to be fully understood. In this paper, we investigate the IF bandwidth of a 0.5 THz all-NbN SIS mixer. First, its IF bandwidth is numerically simulated in terms of the mixer conversion efficiency and time constant. Second, the mixer noise performance is

experimentally characterized in the IF band of 0.5 similar to 12 GHz. Detailed theoretical simulation and experimental results will be presented.

Record 154 of 247

Direct Measurement of the Input RF Noise of Superconducting Hot Electron Bolometer Receivers

Miao, W.; Zhang, W.; Zhou, K. M.; Zhang, K.; Duan, W. Y.; Yao, Q. J.; Shi, S. C.


卷: 23; 期: 3; 页: 2300104-1-2300104-4

A good understanding of input radio-frequency (RF) noise contribution is of particular importance to the development of high-sensitivity superconducting hot electron bolometer (HEB) receivers. In terms of simulation results based on the hot spot model, we found that the output noise of HEB mixers is nearly linearly decreased with the mixer's bath temperature when the HEB mixer is operated at its optimum DC-bias regime under appropriate local-oscillator signal pumping, and the effect of this decrease on the receiver output power can be well corrected. Thus, we used an intersecting lines technique to measure the input RF noise temperature of a quasi-optical superconducting NbN HEB receiver, and the measured input RF noise temperature of the HEB receiver is around 300 K at 850 GHz. For comparison, we also evaluated the losses and equivalent noise temperatures of the quasi-optical components in the RF signal path. The evaluated input RF noise temperature is found to be smaller than the measured one.

Record 155 of 247

Measurement of the spectral response of spiral antenna coupled superconducting hot electron bolometers

Zhang, W.; Miao, W.; Li, S. L.; Zhou, K. M.; Shi, S. C.; Gao, J. R.; Goltsman, G. N.


卷: 23; 期: 3; 页: 2300804-1-2300804-4

Measured spectral response of spiral-antenna coupled superconducting hot electron bolometers (HEBs) often drops dramatically at frequencies that are still within the frequency range of interest (e. g., similar to 5 THz). This is inconsistent with


76

the implied low receiver noise temperatures from the same measurements. To understand this discrepancy, we exhaustively test and calibrate the thermal sources used in Fourier transform spectrometer measurements. We first investigate the absolute emission spectrum of high-pressure Hg arc lamp, then measure the spectral response of two spiral-antenna coupled NbN HEBs with a Martin-Puplett interferometer as spectrometer and 77 K blackbody as broadband signal source. The measured absolute emission spectrum of Hg arc lamp is proportional to frequency, corresponding to an equivalent blackbody temperature of 4000 K at 1 THz, 1500 K at 3 THz, and 800 K at 5 THz, respectively. Measured spectral response of spiral-antenna coupled NbN HEBs, corrected for air absorption, is nearly flat in the frequency range of 0.5-4 THz, consistent with simulated coupling efficiency between HEB and spiral-antenna. These results explain the discrepancy, and prove that spiral-antenna coupled superconducting NbN HEBs work well in a wide frequency range. In addition, this calibration method and these results are broadly applicable to other quasi-optical THz receivers.

Record 156 of 247

Phase-locking of a terahertz solid-state source using a superconducting hot-electron bolometer mixer

Miao, W.; Zhang, W.; Zhou, K. M.; Li, S. L.; Zhang, K.; Duan, W. Y.; Yao, Q. J.; Shi, S. C.

SUPERCONDUCTOR SCIENCE & TECHNOLOGY

卷: 26; 期: 8; 页: 85005-1-85005-4

We report on a scheme whereby the local-oscillator (LO) of a THz heterodyne receiver can be phase-locked by the mixer of the heterodyne receiver. This scheme is demonstrated for the phase-locking of an 847.6 GHz Gunn oscillator and multiplier chain combined source with a superconducting hot-electron bolometer (HEB) mixer. We show that with this technique the phase-locked beat signal can reach a signal-to-noise ratio higher than 70 dB in a resolution bandwidth (RBW) of 1 Hz. This phase-locking scheme should find good use in THz heterodyne spectrometers.

Record 157 of 247

CLOSED-FORM DESIGN FORMULATIONS OF ARBITRARY PHASE DELAY CROSSOVER BASED ON ADMITTANCE MATRIX

Tian, Ge; Yang, Jin-Ping; Wu, Wen

Progress in Electromagnetics Research Letters

卷: 43; 页: 165-173

A design method for four-port crossover with arbitrary phase delay is proposed in this paper. This method is based on admittance matrix. Closed-form design formulations are deduced by making the structure admittance matrix equal to theoretical one. A crossover with 45° phase delay is designed and fabricated for theory veri-cation. In the Butler beam forming network, this crossover has two functions for making the elimination of the 45° phase shifter possible and being used for circuit layout. Thus compact structure and good performance of Butler network can be realized.

Record 158 of 247

A double-jet system in the G31.41 + 0.31 hot molecular core

Moscadelli, L.; Li, J. J.; Cesaroni, R.; Sanna, A.; Xu, Y.; Zhang, Q.


卷: 549; 页: A122-1-A122-22

Context. Many aspects of massive star (greater than or similar to 10 M-circle dot) formation are still unclear. In particular, the outflow properties at close distance (100-1000 AU) from a massive young stellar object (MYSO) are not yet well established. Aims. This work presents a detailed study of the gas kinematics toward the hot molecular core (HMC) G31.41 + 0.31. Methods. To study the HMC 3D kinematics at milli-arcsecond angular resolution, we performed multi-epoch VLBI observations of the H2O 22 GHz and CH3OH 6.7 GHz masers, and single-epoch VLBI of the OH 1.6 GHz masers. Results. Water masers present a symmetric spatial distribution with respect to the HMC center, where two nearby (0.'' 2 apart), compact, VLA sources (labeled "A" and "B") are previously detected. The spatial distribution of a first group of water masers, named "J1", is well fit with an elliptical profile, and the maser proper

Qinhai Observation Station


77

motions mainly diverge from the ellipse center, with average speed of 36 km s(-1). These findings strongly suggest that the "J1" water maser group traces the heads of a young (dynamical time of 1.3 x 10(3) yr), powerful (momentum rate of similar or equal to 0.2 M-circle dot yr(-1) km s(-1)), collimated (semi-opening angle similar or equal to 10 degrees) jet emerging from a MYSO located close (within approximate to 0.'' 15) to the VLA source "B". Most of the water features not belonging to "J1" present an elongated (approximate to 2 '' in size), NE-SW oriented (PA approximate to 70 degrees), S-shape distribution, which we denote with the label "J2". The elongated distribution of the "J2" group and the direction of motion, approximately parallel to the direction of elongation, of most "J2" water masers suggests the presence of another collimated outflow, emitted from a MYSO placed near the VLA source "A". The proper motions of the CH3OH 6.7 GHz masers, mostly diverging from the HMC center, also witness the expansion of the HMC gas driven by the "J1" and "J2" jets. The orientation (PA approximate to 70 degrees) of the "J2" jet agrees well with that (PA = 68 degrees) of the well-defined V-LSR gradient across the HMC revealed by previous interferometric, thermal line observations. Furthermore, the "J2" jet is powerful enough to sustain the large momentum rate, 0.3 M-circle dot yr(-1) km s(-1), estimated from the interferometric, molecular line data in the assumption that the V-LSR gradient represents a collimated outflow. These two facts lead us to favor the interpretation of the V-LSR gradient across the G31.41 + 0.31 HMC in terms of a compact and collimated outflow.

Record 159 of 247

On the hadronic γ-ray emission from Tycho's supernova remnant

Zhang, Xiao; Chen, Yang; Li, Hui; Zhou, Xin


卷: 429; 期: 1; 页: L25-L29

Hadronic gamma-ray emission from supernova remnants (SNRs) is an important tool to test shock acceleration of cosmic-ray protons. Tycho is one of nearly a dozen Galactic SNRs which are suggested to emit hadronic gamma-ray emission. Among them, however, it is the only one in which the hadronic emission is proposed to arise from the interaction with a low-density (similar to 0.3 cm(-3)) ambient medium. Here we present an

alternative hadronic explanation with a modest energy conversion efficiency (of the order of 1 per cent) for this young remnant. With such an efficiency, a normal electron-to-proton ratio (of the order of 10(-2)) is derived from the radio and X-ray synchrotron spectra, and an average ambient density that is at least one order of magnitude higher is derived from the hadronic gamma-ray flux. This result is consistent with the multiband evidence of the presence of a dense medium from the north to the east of the Tycho SNR. The SNR-cloud association, in combination with the H I absorption data, helps to constrain the so-far controversial distance to Tycho and leads to an estimate of 2.5 kpc.

Record 160 of 247

A SEARCH FOR 95 GHz CLASS I METHANOL MASERS IN MOLECULAR OUTFLOWS

Gan, Cong-Gui; Chen, Xi; Shen, Zhi-Qiang; Xu, Ye; Ju, Bing-Gang


卷: 763; 期: 1; 页: 2-1-2-21

We have observed a sample of 288 molecular outflow sources including 123 high-mass and 165 low-mass sources in order to search for class I methanol masers at the 95 GHz transition and to investigate the relationship between outflow characteristics and class I methanol maser emission with the Purple Mountain Observatory 13.7 m radio telescope. Our survey detected 62 sources with 95 GHz methanol masers above a 3 sigma detection limit, which includes 47 high-mass sources and 15 low-mass sources. Therefore, the detection rate is 38% for high-mass outflow sources and 9% for low-mass outflow sources, suggesting that class Imethanol masers are relatively easily excited in high-mass sources. There are 37 newly detected 95 GHz methanol masers (including 27 high-mass and 10 low-mass sources), 19 of which are newly identified (i.e., first identification) class I methanol masers (including 13 high-mass and 6 low-mass sources). A statistical analysis of the distributions of maser detections with the outflow parameters reveals that the maser detection efficiency increases with the outflow properties (e.g., mass, momentum, kinetic energy, mechanical luminosity of outflows, etc.). Systematic investigations of the relationships between the intrinsic luminosity of methanol masers and the outflow properties (including mass, momentum, kinetic energy, bolometric luminosity, and mass-loss rate of the


78

central stellar sources) indicate a positive correlation. This further supports the theory that class I methanol masers are collisionally pumped and associated with shocks when outflows interact with the surrounding ambient medium.

Record 161 of 247

PARALLAXES FOR W49N AND G048.60+0.02: DISTANT STAR FORMING REGIONS IN THE PERSEUS SPIRAL ARM

Zhang, B.; Reid, M. J.; Menten, K. M.; Zheng, X. W.; Brunthaler, A.; Dame, T. M.; Xu, Y.


卷: 775; 期: 1; 页: 79-79-13

We report trigonometric parallax measurements of 22 GHz H2O masers in two massive star-forming regions from Very Long Baseline Array observations as part of the Bar and Spiral Structure Legacy Survey. The distances of 11.11(-0.69)(+0.79) kpc to W49N (G043.16+0.01) and 10.75(-0.55)(+0.61) kpc to G048.60+0.02 locate them in a distant section of the Perseus arm near the solar circle in the first Galactic quadrant. This allows us to locate accurately the inner portion of the Perseus arm for the first time. Combining the present results with sources measured in the outer portion of the arm in the second and third quadrants yields a global pitch angle of 9 degrees.5 +/- 1 degrees.3 for the Perseus arm. We have found almost no H2O maser sources in the Perseus arm for 50 degrees < l < 80 degrees, suggesting that this approximate to 6 kpc section of the arm has little massive star formation activity.

Record 162 of 247

ON THE NATURE OF THE LOCAL SPIRAL ARM OF THE MILKY WAY

Xu, Y.; Li, J. J.; Reid, M. J.; Menten, K. M.; Zheng, X. W.; Brunthaler, A.; Moscadelli, L.; Dame, T. M.; Zhang, B.


卷: 769; 期: 1; 页: 15-1-15-19

Trigonometric parallax measurements of nine water masers associated with the Local Arm of the

Milky Way were carried out as part of the BeSSeL Survey using the Very Long Baseline Array. When combined with 21 other parallax measurements from the literature, the data allow us to study the distribution and three-dimensional motions of star forming regions in the spiral arm over the entire northern sky. Our results suggest that the Local Arm does not have the large pitch angle characteristic of a short spur. Instead its active star formation, overall length (> 5 kpc), and shallow pitch angle (similar to 10 degrees) suggest that it is more like the adjacent Perseus and Sagittarius Arms; perhaps it is a branch of one of these arms. Contrary to previous results, we find the Local Arm to be closer to the Perseus than to the Sagittarius Arm, suggesting that a branching from the former may be more likely. An average peculiar motion of near zero toward both the Galactic center and north Galactic pole, and counter rotation of similar to 5 km s(-1) were observed, indicating that the Local Arm has similar kinematic properties as found for other major spiral arms.

Record 163 of 247

Design Study on Near-Field Radio Holography of the 5-Meter Dome A Terahertz Explorer

Zuo, Yingxi ; Lou, Zheng; Yang, Ji; Cheng, Jingquan

International Symposium on Antennas and Propagation (ISAP)

卷:1;页: 25-28 The 5m Dome A Terahertz Explorer (DATE5) is a proposed terahertz telescope to be deployed in Dome A, Antarctica, to exploit one of the best observing conditions at terahertz wavelengths on earth. In this paper, a design configuration for the near-field holography of the DATE5 surface measurement is presented. Important factors, such as measurement distance, operating frequency, and signal source location, are discussed. Special efforts have been given to the reduction of truncation errors. Simulation results under typical signal-to-noise ratios and design parameters are also provided.


79

III. Applied Celestial Mechanics and Space Object & Debris Research

Record 164 of 247

Frequency Analysis of the Motion of Mars Orbiter Due to Nonspheric Attraction Perturbation

Zhang, Wei; Wang, Xin

Journal of Spacecraft TT & C Technology

卷: 32; 期: 4; 页: 357-362

The analytical solution of Mars orbiter has high significance for study of orbit regularities and on-board computation. Frequency analysis method is used to emulate motion of the Mars orbiter under the Mars non-spherical gravitational perturbation and the result obtained is that the orbit is located in an invariant torus and can be described by the frequency of three angle variables, which is consistent with the KAM theory. High accuracy analytical expression of orbital motion is constructed with numerical method to meet the requirements of long time orbit prediction in on-board computation for space missions. In addition to the capability to give state parameters of the Mars orbiter at any moment, the method can be used to determine the rate of three angle variables and reflect orbit regularities.

Record 165 of 247

A Method of Detecting Space Debris Based on Prior Information

SUN, Rong-yu; ZHANG, Xiao-xiang; ZHAO, Chang-yin


卷: 54; 期: 2; 页: 168-175

A new method for detecting the space debris in image is presented.At first, a gate around the image of object is set with the prior information in this method,and the local background in the gate is calculated;and then several criterions are introduced for the threshold segmentation and object detection;at last,the distance between

object and gate center is obtained with the barycenter method,and the final centroid position of object in the whole frame is obtained by a simple linear translation.To test the effect and efficiency of this method,several tests are carried out.It is demonstrated that this method is simple and convenient for application,and it works fast and robustly,the objects in image can be detected efficiently with high centroid precision.

Record 166 of 247

Scheduling Strategy for Electro-Optical Tracking of Space Objects

Wang, Xin

Journal of Spacecraft TT & C Technology

卷: 32; 期: 1; 页: 89-94

Following analysis of the different characteristics of motion of space objects in different orbits and focusing on orbit arc length, which id a key factor in orbit determination for space object catalog, tracking scheduling optimization models are respectively presented for electro-optical tracking of low and high altitude objects based on linear programming. Simulation shows that the optimization models maximize the total orbit arc length by eliminating tracking schedule conflicts. Moreover, the computation cost meets the requirements of operational observation. Experoments show that the scheduling method is effective and practical, and oncreases observation time by around 50%.

Record 167 of 247

The Bootstrap Estimation of the Accuracy of Preliminary Orbit Determination

Wang, Xin


卷: 54; 期: 1; 页: 73-78

From the point of view of the non-parametric statistics, a general estimation method of accuracy and confidence interval of the preliminary orbit determination is proposed for the occasion without any other information. The

Center for Space Object and Debris

Research


80

method, based on the bootstrap method, employs only observation data with minimal assumptions about the distributions of observational noise and does not require the result of precise orbit determination as a reference. Numerical check shows that the method is very easy in implementation, and the estimation result is beneficial for both the evaluation of accuracy and follow-up inference.

Record 168 of 247

Design and Implementation of CNEOST Image Database Based on NoSQL System

Wang, Xin


卷: 54; 期: 4; 页: 382-391

The China Near Earth Object Survey Telescope(CNEOST) is the largest Schmidt telescope in China,and it has acquired more than 3 TB astronomical image data since it saw the first light in 2006.After the upgradation of the CCD camera in 2013,over 10 TB data will be obtained every year.The management of massive images is not only an indispensable part of data processing pipeline but also the basis of data sharing.Based on the analysis of requirement,an image management system is designed and implemented by employing the non-relational database.

Record 169 of 247

A Robust Method of Preliminary Orbit Determination

Wang, Xin


卷: 54; 期: 3; 页: 274-281

The preliminary orbit determination with optical angular measurements plays an important role in the survey of space object. The classical method of orbit computing, based on least square error estimation is not robust while the outliers occur in the observation. A robust method is proposed by employing the least absolute deviation estimation. The method reduces the problem of orbit computing to a linear programming problem, and gives the variance of the estimation with bootstrap method. Numerical check shows that the method is effective as well as robust, and has a high breskdown point.

Record 170 of 247

A Modified Gooding's Method to Calculate Inclination Function

Wu, Lianda; Wang, Hongbo


卷: 54; 期: 1; 页: 62-68

In this paper, the V_(lm)~k(I) in Gooding's method is rewritten to the convenient form for calculation, and a standard procedure is used to calculate the V_(lm)~k(I). We rewrite the Gooding's program in the case l and k have the same odd-even parity, cutting a half of the computing program. Then the accuracy and stability of this program are improved, and the computing time is 41% less than Gooding's.

Record 171 of 247

A Method to Calculate Inclination Function with Jacobi Polynomials

Wu Lianda; Wang Hongbo; Ma Jingyuan


卷: 54; 期: 1; 页: 49-58

In this paper, a method to calculate the inclination function with Jacobi polynomials is introduced. Its expressions are very simple. With this method, it is unnecessary to distinguish whether k and l have the same parity, to calculate the non-integral

factorial, and to convert from k < 0 to k≧ 0. We can use the standard Jacobi polynomial program to compute inclination function. Its accuracy is the same as Gooding's method, and the computing time is 9% less than Gooding's.

Record 172 of 247

The Comparison between Two Methods to Calculate Inclination Function with d-function



卷: 54; 期: 2; 页: 147-160

Using the Blanco's recursion relation and Risbo's recursion relation of d-function, we can obtain two methods to calculate the inclination function: d-funl and d-fun2. These two methods are both with high precision and high stability. The precision of d-fun2 is better than d-funl's for small inclination. But for other inclinations, d-funl is better. The stability of d-fun2 is obviously better than d-funl's, and the computation speed of d-funl is seven times faster than d-fun2's. Both methods


81

have a singularity with sin I=0. Besides, the resulted indication functions calculated with both methods are normalized, and the computation of inclination function without singularity can not be realized. Therefore, these methods might not be used in the motion theory of non-singularity elements.

Record 173 of 247

A Research on a Special Singularity of Recursion Formulae in Inclination Function Computation



卷: 54; 期: 2; 页: 161-167

For deriving the formulae of inclination function of iota-recursion and p-recursion, the following recursion function relations are often used: A_1A_(iota-l,m,p)(I)+A_2A_(iota,m,p)(I)+A_3A_(iota-l,m,p)(I)=0 and C_1A_(iota,m,p-l)(I)+C_2A_(iota,m,p)(I)+=C_3A_(iota,m,p)(I)=0.In this aper, we point out that these equations will result in the inclusion of a special singularity with cos I = 1/n (n is an integer) in the recursion formulae of inclination function, and some errors would appear in the computation results. Using another recursion function relations, this special singularity can be avoided.

Record 174 of 247

A Quad-precision Calculation Test for Inclination Function



卷: 54; 期: 3; 页: 235-244

In the analytical theories of celestial mechanics, the inclination function is a kind of frequently-used function when we expand the perturbation function as a form of time and orbit elements. A lot of classic recursion methods were brought out in history, and their Fortran-code were developed on the double-precision computer platform. While in this paper, a test of quad-precision calculation are reported. The results show that the quad-precision calculation precision of the L-plane recursion method can reach 10~(-22), and its computation speed is six times faster than the double-precision calculation of Jacobi method.

Record 175 of 247

Stability Analysis of Recursion Relation for Inclination Function



卷: 54; 期: 3; 页: 229-234

Many kinds of recursion methods of inclination function had been brought out in history. However, several methods were found to be unstable in the high order. By the magnitude analysis of inclination functions in the direction of recursion, the stability of the recursion relation of inclination function can be estimated. For the commonly-used three-term recursion, only the M_k(l) recursion is stable, the others are unstable. But the stability of the multi-term recursion is more complex, it is necessary to make an in-depth analysis.

Record 176 of 247

Analysis of the applicability of collision probability algorithms for nonlinear relative motion

Xu XiaoLi; Xiong YongQing


卷: 56; 期: 5; 页: 1041-1046

In the calculation of the collision probability between space objects, the assumption of linear relative motion is generally adopted to simplify the problem because most encounters are at high relative velocity. Nevertheless, the assumption is no longer valid for encounters at extremely low velocities, and a new algorithm is urgently needed for computing collision probability for space objects having nonlinear relative motion. In this particular case, the direction associated with relative velocity is reintroduced for integration. The different integral limits would lead to the variations of probability and integral time. Moreover, the application scope of this new algorithm is also presented. Since the nonlinear effect is only significant in some certain situations, the new algorithm needs to be considered only in such certain situations. More specifically, when space objects in circular orbits encounter with a tiny inclined angle (the extreme situation), the new algorithm can derive much more accurate collision probability than the linear method, that is to say, the linearity assumption involved in general collision probability formulation is not


82

adequate anymore. In addition, the deviation of the probability derived by the linear method (linear collision probability) from that derived by the nonlinear method (nonlinear collision probability) also weakly depends on the relative distance and combined covariance, and essentially depends on their ratio.

Record 177 of 247

The unified ideal model of mean motion resonance of artificial satellites due to geopotential perturbations

Zhang MingJiang; Zhao ChangYin; Xiong YongQing; Sun RongYu; Zhu TingLei


卷: 56; 期: 4; 页: 840-847

From Kaula's Earth gravitational potential written in classical orbital elements, the unified ideal model of mean motion resonance of artificial satellites due to geopotential perturbations is developed in this paper first, through a suitable sequence of canonical transformations constructed by implicit functions. This unified ideal orbital resonance model is valid for all the commensurabilities between the rotational angular velocity of the Earth and the angular velocities of mean orbital motion of artificial satellites with arbitrary inclination and small eccentricity, and can be also transformed into Garfinkel's general expression of ideal resonance problem. Then 1/1 resonance of the 24-hour satellite with arbitrary inclination and small eccentricity is analyzed under the effect of harmonics of J (2) and J (22) of the geopotential, based on the unified ideal model of mean motion resonance. The analytical expressions of the libration period and libration half width of the 1/1 resonance of the 24-hour satellite with arbitrary inclination and small eccentricity are presented.

Record 178 of 247

Dynamical evolution of high area-to-mass ratio objects in Molniya orbits

Sun, Rong-yu; Zhao, Chang-yin; Zhang, Ming-jiang; Hou, Yong-Gang

ADVANCES IN SPACE RESEARCH

卷: 51; 期: 11; 页: 2136-2144

For special demands, some notable orbit types have been developed by human, including the

Molniya orbits, which have a relatively high eccentricity up to about 0.7, and a period of 12 h. Considering that space debris with high area-to-mass ratio (A/M) has been discovered, such objects may also exist in Molniya orbits due to spacecraft and upper stages fragmentation events. However, there are not sufficient studies of the complex dynamical phenomena of such orbits. These studies can enrich the knowledge about the long-term evolution of these orbits, be helpful to propose uncatalogued objects observation and identification, and also set the protected region as well as active debris removal. In this paper, the characteristics of 2:1 resonance of Molniya satellite orbits are studied. A large set of numerical simulations, including all the relevant perturbations, is carried out to further investigate the main characteristics, and special attention is payed to the dynamical evolution of objects with high A/M, particularly affected by the direct solar radiation pressure. The long-term dynamical evolution of orbital elements, as well as the dependency of lifetime on the A/M value, is discussed.

Record 179 of 247

Two-dimensional phase plane structure and the stability of the orbital motion for space debris in the geosynchronous ring

Zhao, Chang-Yin; Zhang, Ming-Jiang; Wang, Hong-Bo; Zhang, Wei; Xiong, Jian-Ning


卷: 52; 期: 4; 页: 677-684

Based on the orbital resonance model, we study the two-dimensional phase plane structure of the motion of space debris orbiting the geosynchronous ring under the combined effects of the tesseral harmonics J(22), J(31) and J(33) of the Earth's gravitational field. We present the main characteristic parameters of the two-dimensional phase plane structure. We also analyze the stability of the two-dimensional phase plane structure with numerical method. Our main findings indicate that the combined effects of the tesseral harmonics J(22), J(31) and J(33) fully determine the two-dimensional phase plane structure of the space debris, and it remains robust under the effect of the Earth's actual gravitational field, the luni-solar perturbations and the solar radiation pressure with the normal area-to-mass ratios.


83

Record 180 of 247

A new source extraction algorithm for optical space debris observation

Sun, Rong-Yu; Zhao, Chang-Yin


卷: 13; 期: 5; 页: 604-614

Specific challenges arise in the task of real-time automatic data reduction of optical space debris observations. Here we present an automatic technique that optimally detects and measures the sources from images of optical space debris observations. We show that highly reliable and accurate results can be obtained on most images produced by our specific sensors, and due to optimizations, the whole pipeline works fast and efficiently. Tests demonstrate that the technique performs better than SExtractor from the point of view of fast and accurate detection, therefore it is well suited for data reduction of optical space debris observations.

Record 181 of 247

An innovative image reconstruction method for high precision astrometry

Sun, Rong-Yu; Zhao, Chang-Yin; Zhang, Yi-Ping

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN

卷: 65; 期: 5; 页: 110-1-110-9

An automatic image-reconstruction method is presented, based on the use of a mathematical morphology operator. Variable structural elements along multiple directions are adopted for image convolution, and then all of the corresponding convolved images are stacked to obtain a final result. To investigate its efficiency, both simulated images and raw CCD images, produced by a trial observation using a 45-cm telescope, are tested. With this method, the influence of degradation in astrometric CCD images is reduced, and the position accuracy of background stars is distinctly improved. This method will contribute significantly to optical data reduction and high-order precision astrometry.

Record 182 of 247

北斗导航卫星同步轨道的共振特性及长期演化

侯永刚; 赵长印; 孙荣煜

第四届中国卫星导航学术年会

页: 1-5

到目前为止，有 3 颗北斗导航卫星处于倾斜同步

轨道上，其轨道倾角为55o，轨道偏心率为0.003。

同步轨道与地球非球形引力势的田谐项会产生

强烈的 1:1 共振，而且倾斜同步轨道因为轨道倾

角比较大，在考虑共振时需要考虑的田谐项更多，

处理过程也更复杂。有特殊轨道倾角(55o 是其

中之一)的轨道会在地球非球形引力 J2 项的影响

下，产生近心点角踞和升交点经度两个轨道根数

之间的共振作用。这 3 颗北斗通信卫星均是处于

双重共振的作用下，这种共振对卫星的长期演化

有重要作用。本文从经典的考拉地球非球形引力

势方程出发,用德洛内根数表示出哈密顿方程后，

通过三次正则变换将哈密顿方程转换成理想共

振的形式，然后对比与单摆模型得到北斗轨道的

稳定点和稳定点周围的运动状态。高轨卫星受到

的摄动除了非球形引力的 J2 项以外最大的便是

日月第三体引力摄动,本文将日月三体对北斗卫

星轨道的哈密顿函数加入到地球引力函数中，平

均化之后解出一阶摄动解，并且得出其对双重共

振的影响。最后对三个轨道做数值验证。

Record 183 of 247

Searching for space debris in GEO

Sun, RongYu; Zhao, ChangYin

第七届全国空间碎片学术交流会

期: 1; 页: 52-58

A method combined with geometrical morphology identification and linear correlation is adopted for the data calibration of IADC (the Inter-Agency Space Debris Coordination Committee) AI23.4. The main aim for this action is detecting the debris in GEO region. During calibration, the pointing errors of telescope are corrected, and 1137 detections are obtained from the raw CCD images. Finally 139 tracklets are acquired, of which 116 tracklets are correlated with the catalogue. The distributions of magnitude, semi-major axis, inclination and longitude of ascending node of these objects are obtained as well.

Record 184 of 247

加权最小二乘在精密天文定位中的应用

孙荣煜; 赵长印; 侯永刚

第四届中国卫星导航学术年会

传统天文定位方法采用底片常数模型，计算图像

坐标与理想坐标的映射关系，最终实现图像坐标

与赤道坐标的转换。其在光学测角资料的处理，

星敏感器指向的归算中有广泛的应用。天文定位


84

方法的实质为计算线性方程组的最小二乘解。实

际处理过程中，恒星质心坐标的测量误差，定标

星匹配错误，以及定标星数目不足等因素导致天

文定位的精度降低。为了解决以上问题，实现高

精度的天文定位，使用最优加权的最小二乘方法

计算底片常数。试验结果表明，该方法降低了恒

星位置误差对结果的影响，剔除了定标星的偶然

匹配误差，提高了定位的精度，并能在定标星数

目不够的情况下实现天文定位。因此，提高了观

测数据利用效率以及观测的精度，在实际工作中

有较高的应用价值。

Record 185 of 247

Space Objects Photometry Using Optical Telescope Array

Zhang, Chen; Ping, Yiding; Zhao, Changyin

Space Debris Research

期: 1; 页: 28-31

This paper summarizes the recent analysis work on space objects photometry using optical telescope array. With this work, we can understand the accuracy of the data better, and correct the data to make it available for application.

Record 186 of 247

The long-term evolution of the plane of GEO disposal orbits

ZHANG, Mingjiang; ZHAO, Changyin; WANG,

Hongbo; SUN, Rongyu

第七届全国空间碎片学术交流会论文

期: 1; 页: 997-1004

The Inter-Agency Space Debris Coordination Committee (IADC) proposed the specific requirements on the GEO satellite disposal orbit in its “IADC Space Debris Mitigation Guidelines”. The GEO satellite disposal orbit must have an eccentricity less than or equal to 0.003, which can be regarded as a circular orbit approximately. Base on Allan and Cook’s theory of the long-period motion of the plane of a distant circular orbit under the effect of the second zonal harmonic of the Earth’s gravitational potential and the second harmonics of the luni-solar perturbations by a vector method, the long-term evolution of the plane of GEO disposal orbits is further investigated under the assumption of circular orbit in this paper. The long-term evolution relationship between the inclination and the longitude of ascending node of a series of GEO disposal orbits with different initial conditions are presented. The corresponding results obtained by the theoretical analysis are verified through long-term numerical integrations under the actual effect of the Earth’s gravitational potential, the luni-solar perturbations and the solar radiation pressure.


85

IV. Planetary Sciences and Deep Space Exploration

Record 187 of 247

Numerical simulation of time delay interferometry for a LISA-like mission with the simplification of having only one interferometer

Dhurandhar, S. V.; Ni, W. -T.; Wang, G.


卷: 51; 期: 1; 页: 198-206

In order to attain the requisite sensitivity for LISA, laser frequency noise must be suppressed below the secondary noises such as the optical path noise, acceleration noise etc. In a previous paper (Dhurandhar, S.V., Nayak, K.R., Vinet, J.-Y. Time delay interferometry for LISA with one arm dysfunctional. Class. Quantum Gray. 27, 135013, 2010), we have found a large family of second-generation analytic solutions of time delay interferometry with one arm dysfunctional, and we also estimated the laser noise due to residual time-delay semi-analytically from orbit perturbations due to Earth. Since other planets and solar-system bodies also perturb the orbits of LISA spacecraft and affect the time delay interferometry (TDI), we simulate the time delay numerically in this paper for all solutions with the generation number n <= 3. We have worked out a set of 3-year optimized mission orbits of LISA spacecraft starting at January 1, 2021 using the CGC2.7 ephemeris framework. We then use this numerical solution to calculate the residual optical path differences in the second-generation solutions of our previous paper, and compare with the semi-analytic error estimate. The accuracy of this calculation is better than 1 cm (or 30 ps). The maximum path length difference, for all configuration calculated, is below 1 m (3 ns). This is well below the limit under which the laser frequency noise is required to be suppressed. The numerical simulation in this paper can be applied to other space-borne interferometers for gravitational wave detection with the

simplification of having only one interferometer.

Record 188 of 247

Comparisons and Evalustions of JPL Ephemerides

Deng, Xue-Mei; Fan, Min; Xie, Yi


卷: 54; 期: 6; 页: 550-561

Since NASA’s JPL (Jet Propulsion Laboratory) Ephemerides are widely used in deep space navigation and planetary exploration, it is necessary to compare their details, including the coverage, realization and maintenance. Focusing on Chinese Venus and Mars missions in the future, we take DE405, DE421, and DE423 as samples to analyze their dynamical models and observation data. By evaluating their accuracies and performances, we investigate their effects on an orbiter around Venus and Mars, and recommend that it is better to use DE423 for Venus missions and DE421/DE423 for Mars missions.

Record 189 of 247

The mid-term and long-term solar quasi-periodic cycles and the possible relationship with planetary motions

Tan, Baolin; Cheng, Zhuo


卷: 343; 期: 2; 页: 511-521

This work investigates the solar quasi-periodic cycles with multi-timescales and the possible relationships with planetary motions. The solar cycles are derived from long-term observations of the relative sunspot number and microwave emission at frequency of 2.80 GHz. A series of solar quasi-periodic cycles with multi-timescales are registered. These cycles can be classified into three classes: (1) the strong PLC (PLC is defined as

Ephemerial Astronomy and Astronomical

Reference System

Near Earth Object Survey and Solar

System Bodies


86

the solar cycle with a period very close to the ones of some planetary motions, named as planetary-like cycle) which is related strongly with planetary motions, including nine periodic modes with relatively short period (P < 12 yr), and related to the motions of the inner planets and of Jupiter; (2) the weak PLC, which is related weakly to planetary motions, including two periodic modes with relatively long period (P > 12 yr), and possibly related to the motions of outer planets; (3) the non-PLC, for which so far there has been found no clear evidence to show the relationship with any planetary motions. Among the planets, Jupiter plays a key role in most periodic modes due to its sidereal motion or spring tidal motions associated with other planets. Among planetary motions, the spring tidal motion of the inner planets and of Jupiter dominates the formation of most PLCs. The relationships between multi-timescale solar periodic modes and the planetary motions will help us to understand the essential nature and prediction of solar activities.

Record 190 of 247

On preference of Yoshida construction over Forest-Ruth fourth-order symplectic algorithm

Mei, Lijie; Wu, Xin; Liu, Fuyao

EUROPEAN PHYSICAL JOURNAL C

卷: 73; 期: 6; 页: 2413-1-2413-8

The Forest-Ruth fourth-order symplectic algorithm is identical to the Yoshida triplet construction when all component integrators of both algorithms are exactly known. However, this equality no longer holds in general when some or all of the components are inexact and when they are second-order with odd-order error structures. The former algorithm is only second-order accurate in most cases, whereas the latter can be fourth-order accurate. These analytical results are supported by numerical simulations of partially separable but globally inseparable Hamiltonian systems, such as the post-Newtonian Hamiltonian formulation of spinless compact binaries. Therefore, the Yoshida construction has intrinsic merit over the concatenated Forest-Ruth algorithm when inexact component integrators are used.

Record 191 of 247

f (T) gravity: effects on astronomical observations and Solar system experiments and upper bounds

Xie, Yi; Deng, Xue-Mei


卷: 433; 期: 4; 页: 3584-3589

The effects of the f (T) gravity have previously been investigated and constrained by using perihelion advances. As an extension of previous work and as an attempt to find more stringent constraints on its parameters, we investigate here its effects on astronomical observations and on experiments conducted in the Solar system. The expression for f (T) contains a quadratic correction of alpha*T-2 (where alpha is a model parameter) and the cosmological constant Lambda. Using a spherical solution describing the Sun's gravitational field, the resulting secular evolution of planetary orbital motions, in addition to the light deflection, gravitational time delay and frequency shift are calculated up to the leading contribution. From these results, we find qualitatively that the light deflection provides a unique bound on alpha, without dependence on Lambda, and that the time delay experiments during inferior conjunction impose a clean constraint on Lambda, regardless of alpha. Based on observations and experiments, especially the supplementary advances in the perihelia provided by the INPOP10a ephemeris, we obtain the upper bounds quantitatively: vertical bar alpha vertical bar < 1.2 x 10(2) m(2) and vertical bar Lambda vertical bar < 1.8 x 10(-43) m(-2), which are at least 10 times tighter than the previous results.

Record 192 of 247

Dynamics of spin effects of compact binaries

Mei, Lijie; Ju, Mingjie; Wu, Xin; Liu, Sanqiu


卷: 435; 期: 3; 页: 2246-2255

For a 10-dimensional post-Newtonian canonical conservative Hamiltonian system of spinning compact binaries, where the orbital part is accurate to the third-order post-Newtonian expansion and the spin-orbit contributions are up to the next-to-next-to-leading order, its dynamics is integrable and not at all chaotic due to the presence of five independent isolating integrals, including the total energy, three components of


87

the total angular momentum vector and the length of the orbital angular momentum. As the spin-spin effects of the two spinning bodies are further included, only the length of the orbital angular momentum is no longer conserved, so that the dynamics becomes typically non-integrable. Numerical simulations support the onset of chaos. Above all, many chaotic orbits whose initial radii are larger than 10M and whose Lyapunov times are less than the corresponding inspiral decay times are found. In addition, a threshold value of the maximum ratio of the spin-spin Hamiltonian to the whole Hamiltonian for distinguishing between the ordered and chaotic cases is also given.

Record 193 of 247

The effect of f(T) gravity on an interplanetary clock and its time transfer link

Deng, Xue-Mei; Xie, Yi


卷: 13; 期: 10; 页: 1225-1230

As an extension of the "teleparallel" equivalent of general relativity, f(T) gravity is proposed to explain some puzzling cosmological behaviors, such as accelerating expansion of the Universe. Given the fact that modified gravity also has impacts on the Solar System, we might test it during future interplanetary missions with ultra-stable clocks. In this work, we investigate the effects of f(T) gravity on the dynamics of the clock and its time transfer link. Under these influences, the Lambda-term and the alpha-term of f(T) gravity play important roles. Here, Lambda is the cosmological constant and alpha represents a model parameter in f(T) gravity that determines the divergence from teleparallel gravity at the first order approximation. We find that the signal of f(T) gravity in the time transfer is much more difficult to detect with the current state of development for clocks than those effects on dynamics of an interplanetary spacecraft with a bounded orbit with parameters 0.5 au <= a <= 5.5 au and 0 <= e <= 0.1.

Record 194 of 247

HIPPARCOS PHOTOCENTRIC ORBITS OF 72 SINGLE-LINED SPECTROSCOPIC BINARIES

Ren, Shulin; Fu, Yanning


卷: 145; 期: 3; 页: 81-1-81-7

By fitting the Hipparcos Intermediate Astrometric Data (HIAD), photocentric orbits can be obtained for the single-lined spectroscopic binaries (SB1s). In previous work, a simplifying approximation used in the fitting process was that the photocenter coincides with the primary, but simple arguments based on a mass-luminosity relation show that this approximation will introduce non-negligible deviation into photocentric orbits of a few SB1s. By fitting the revised HIAD without the approximation, the present paper tries to provide reliable photocentric orbits for those SB1s in the 9th Catalogue of Orbits of Spectroscopic Binaries having a reliable spectroscopic orbit of period between 50 days and 3.2 years. After a stringent assessment and screening process, we finally accept the photocentric orbits of 72 systems. Among these results, 37 orbits are obtained here for the first time. So far, only three of these systems are resolved with a known relative orbit. For each of them, the paired photocentric and relative orbits are in reasonably good agreement. For the 25 systems with a main-sequence primary, the masses of component stars and the semimajor axes of relative orbits are estimated for the purpose of planning ground-based observations.

Record 195 of 247

Yukawa effects on the clock onboard a drag-free satellite

Deng, Xue-Mei; Xie, Yi


卷: 431; 期: 4; 页: 3236-3239

The Yukawa correction to the Newtonian gravitational force is accepted as a parametrization of deviations from the inverse-square law of gravity which might be caused by new physics beyond the standard model of particles and the general theory of relativity. We investigate these effects on the clock onboard a drag-free satellite: dynamics of the satellite and influence on the time transfer link. We find that the Yukawa signal in the time transfer is much more difficult to detect with the current state of clocks than those effects on the dynamics, especially the secular change of periastron, by laser ranging in the case of an artificial Earth satellite carrying a frequency standard with an orbit of a = 10(7) m and e = 0.01.


88

Record 196 of 247

Possible Yukawa gravity effects on time transfer between the Earth and Satellites

Deng, Xue-Mei

2013 年全国时间频率学术会议论文集

期: 10; 页: 471-475

The Yukawa corrention to the Newtonian gravitational force is accepted as a patametrization of deviations from the inverse-square law of gravity which might be caused by new physics beyond the standard model of particles and the general theory of relativity. We investigate these effects on the clock onboard a drag-free satellite: dynamics of the satellite and influence on the time transfer link. We find that the Yukawa signal in the time transfer is much more difficult to detect with the current state of clocks than those effects on the dynamics, especially the secular change of periastron, by laser ranging in the xase of an artificial Earth satellite carrying a frequency standard with an orbit of a=10

7 m and e=0.01.

Record 197 of 247

美国喷气推进实验室不同版本行星历表的比较

Deng, Xue-Mei

中国宇航学会深空探测技术专业委员会第十届

学术年会论文集

期: 10; 页: 247-239

本文针对美国宇航局喷气推进实验室研发的系

列行星历表,就其内容、适用范围、实现和维护

进行了比较。针对我国有望开展的火星和金星深

空探测任务，着重评估了其不同版本历表的精度

和性能，给出了使用上的建议。

Record 198 of 247

Constraints on Yukawa parameters by double pulsars

Deng, Xue-Mei; Xie, Yi; Huang, Tian-Yi


卷: 8; 页: 372-374

Although Einstein's general relativity has passed all the tests so far, alternative theories are still required for deeper understanding of the nature of gravity. Double pulsars provide us a significant opportunity to test them. In order to probe some modified gravities which try to explain some

astrophysical phenomena without dark matter, we use periastron advance dot{ω} of four binary pulsars (PSR B1913+16, PSR B1534+12, PSR J0737-3039 and PSR B2127+11C) to constrain their Yukawa parameters: λ = (3.97 ± 0.01) × 10

8m

and α = (2.40 ± 0.02) × 10-8

. It might help us to distinguish different gravity theories and get closer to the new physics.

Record 199 of 247

Linear Stability of the n-gon Relative Equilibria of the (1+n)-Body Problem

Xu, Xingbo;

QUALITATIVE THEORY OF DYNAMICAL SYSTEMS

卷:12;期:1;页: 255-271; 特刊: SI We consider the linear stability of the regular n-gon relative equilibria of the (1 + n)-body problem. It is shown that there exist at most two kinds of infinitesimal bodies arranged alternatively at the vertices of a regular n-gon when n is even, and only one set of identical infinitesimal bodies when n is odd. In the case of n even, the regular n-gon relative equilibrium is shown to be linearly stable when n >= 14. In each case of n = 8, 10 and 12, linear stability can also be preserved if the ratio of two kinds of masses belongs to an open interval. When n is odd, the related conclusion on the linear stability is recalled.

Record 200 of 247

磁流体力学之父—阿尔文

李兵

力学与实践

卷: 35; 期: 6; 页: 97-99

阿尔文以他深刻的洞察力和敏锐的物理直觉改

变了我们对宇宙的传统看法，他一系列开创性的

工作使得磁流体力学真正成为现代物理学的一

个重要分支。单介绍了阿尔文的主要学术成就以

及学术遭遇，并对其辉煌成就、学术遭遇背后可

能的原因做了简要分析。

Record 201 of 247

The Sun and Solar System Plasmas


89

Experimental Studies of Kinetic Alfven Waves

Wu, De-Jin; Chen, Ling

Progress in Physics

卷: 33; 期: 2; 页: 57-85

Kinetic Alfvén waves(KAWs hereafter),dispersive Alfvén waves with a short perpendicular wavelength comparable to the ion gyroradius or the electron inertial length,have been an increasingly interesting subject in space and laboratory plasmas because it can play an important role in the formation of filamentous fine-structures and the energization of charged particles in magneto-plasmas.In particular,since 1990’s advances in both space-and ground-based experimental techniques have led to a series of great and important progresses in experimental study of KAWs.These experimental studies not only confirmed many essential,significant,and interesting features of KAWs predicted by theories,but also led to the reevaluation of the importance of KAWs in the magneto-plasma dynamics and remotivated studying interest of KAWs in various magneto-plasma phenomena from laboratory to space and astrophysical plasmas.This paper presents a review of experimental studies of KAWs,including plasma experiments on large plasma devices in laboratory,in situ measurements by satellites in space plasmas from the magnetosphere to the solar wind,and remote observations from the solar atmosphere.These experimental studies cover various aspects of KAW physics,including their basic dispersion relations,electromagnetic polarization states,excitation and dissipation mechanisms,nonlinear interaction phenomena,and turbulence spectra in various plasma environments.This review is particularly helpful for readers to understand comprehensively KAW physics and KAW-related phenomena.

Record 202 of 247

The Dynamics of Beam-return Current Systems in the Solar Atmosphere

XU, Lei; WU, Dejin

Progress in Astronomy

卷: 31; 期: 2; 页: 160-184

Beams of energetic charged particles are a common product from a variety of astrophysical activities. These beams may be naturally accompanied by return currents to maintain

charge neutrality and zero-current. Their propagation in cosmic plasmas in general, and the dynamics of the beam-return current system in particular, have been under intensive investigation as a fundamental problem in astrophysics. On the other hand, the multi-wavelength, high-resolution observations of solar activities, observations of the solar wind and of Earths ionosphere that have been routinely made recently offer a rich set of data on which theoretical studies can be built. After briefly reviewing the historical development of the investigations into the dynamics of the beam-return current system in a solar atmosphere, we present an overview of the recent developments in the theories on how the return current is generated, in examining the instabilities such a system may be subjected to, and in the numerical simulations as well as data analyses of such a system. We conclude by pointing out some possible directions that are worth pursuing in this field.

Record 203 of 247

Electron cyclotron maser emission in the coronal arch as the source of Type V bursts

Tang, JianFei; Wu, DeJin; Tan, C. M.

Astrophysical Journal

卷: 779; 期: 1; 页: 83-1-83-7

Solar radio type V bursts were classified as a special spectral class based on their moderately long duration, wide bandwidth, and sense of polarization opposite of associated type III bursts. However, type V bursts are also closely related to the preceding type III bursts. They have an approximately equal source height and the same dispersion of position with frequency. Electron cyclotron maser (ECM) instability driven by beam electrons has been used to explain type III bursts in recent years. We propose ECM emission as the physical process of type V solar radio bursts. According to the observed properties of type V and III bursts, we propose that energetic electrons in excited type V continuum are trapped in coronal loops, which are adjacent to the open field lines traced by type III electrons. With the proposed magnetic field configuration and the ECM emission mechanism, the observed properties of type V bursts, such as long duration, wide bandwidth, and opposite sense of polarization can be reasonably explained by our model.


90

Record 204 of 247

On the possibility of spontaneous generation of turbulent Alfven waves in solar plasma by heavy ions

Wu, C. S.; Zhao, G. Q.; Chen, L.; Wu, D. J.

PHYSICS OF PLASMAS

卷: 20; 期: 8; 页: 082102

In this paper, we discuss spontaneous generation of Alfven waves. The discussion is motivated by the study of the solar transition region. We show that the heavy ions in this region can play critical roles. A quasilinear theory is derived. On the basis of this theory, we can discuss the saturation level of the wave spectral energy associated with each species of ions. Several essential issues relevant to the transition region are also discussed. (C) 2013 AIP Publishing LLC.

Record 205 of 247

Emission of radiation induced by pervading Alfven waves

Zhao, G. Q.; Wu, C. S.

PHYSICS OF PLASMAS

卷: 20; 期: 3; 页: 34503-1-34503-4

It is shown that under certain conditions, propagating Alfven waves can energize electrons so that consequently a new cyclotron maser instability is born. The necessary condition is that the plasma frequency is lower than electron gyrofrequency. This condition implies high Alfven speed, which can pitch-angle scatter electrons effectively and therefore the electrons are able to acquire free energy which are needed for the instability.

Record 206 of 247

Nonlinear interaction and parametric instability of kinetic Alfven waves in multicomponent plasmas

Zhao, J. S.; Wu, D. J.; Yang, L.; Lu, J. Y.

PHYSICS OF PLASMAS

卷: 20; 期: 3; 页: 32308-1-32308-6

Nonlinear couplings among kinetic Alfven waves are investigated for a three-component plasma consisting of electrons, protons, and heavy ions. The parametric instability is investigated, and the growth rate is obtained. In the kinetic regime, the growth rate for the parallel decay instability

increases with the heavy ion content, but the growth rate for the reverse decay is independent of the latter since the perpendicular wavelength is much larger than the ion gyroradius. It decreases with the heavy ion content when the perpendicular wavelength is of the order of the ion gyroradius. It is also found that in the short perpendicular wavelength limit, the growth rate is only weakly affected by the heavy ions. On the other hand, in the inertial regime, for both parallel and reverse decay cases, the growth rate decreases as the number of heavy ions becomes large.

Record 207 of 247

Kinetic Alfvén wave instability driven by field-aligned currents in a low-beta plasma

Chen, L.; Wu, D. J.; Huang, J.

Journal of Geophysical Research: Space Physics

卷: 118; 期: 6; 页: 2951-2957

Kinetic Alfvén waves (KAWs) can play an important role in the energization of plasma particles and the formation of filamentous structures, which commonly are encountered and frequently accompanied by field-aligned currents in various magneto-plasmas, such as laboratory, auroral, and coronal plasmas. Based on a low-frequency kinetic dispersion equation in frequency ω < ωci (the ion cyclotron frequency), KAW instability driven by a field-aligned current, which is carried by the field-aligned drift of electrons at velocity VD, is investigated in a low-β plasma of β < Q << 1, where β is the kinetic-to-magnetic pressure ratio and Q (≡ me/mi << 1) is the mass ratio of electrons to ions. An instability condition and the corresponding growth rate are obtained, which depends on the plasma β parameter as well as the drift velocity VD. The results show that the KAW instability occurs in the perpendicular wave number of

, in which the growth rate reaches

its maximum at for fixed VD and β. As VD increases, this growing wave number range widens and the growth rate increases, but the

maximal-growing wave number decreases. On the other hand, as the plasma βparameter decreases, the growing wave number range also widens, and the maximal-growing wave number and growth rate both increase. These results have potential importance in understanding the physics of the electric current dissipation and plasma active phenomena since the field-aligned current


91

is one of the most active factors in space and astrophysical plasmas.

Record 208 of 247

Anomalous resistivity in beam-return currents and hard-X ray spectra of solar flares

Xu, L.; Chen, L.; Wu, D. J.


卷: 550; 页: A63-1-A63-6

Context. Observations of hard-X ray (HXR) spectra from solar flares show that there is noncollisional energy loss when energetic beam electrons are transported along the flare loop from their acceleration site above the looptop in the corona to the loop footpoints in the chromosphere. Aims. This paper investigates anomalous (i.e., noncollisional) resistivity due to the effective collision by the wave-particle interaction in the beam-return current system of a flare and its effect on the HXR spectral evolution between the looptop and footpoint sources. Methods. To attribute the noncollisional energy loss to an induced electric field by the beam current, the induced electric field is estimated by the spectral evolution between the looptop and footpoint sources, which is deduced from the standard thin-thick target model. To include collisional and anomalous resistivity caused by the ion-acoustic wave turbulence excited by the return current, the necessary excited level and the excited condition are discussed for the steady-state case in which the return current density driven by the induced electric field in terms of Ohm's law is required to be equal to the beam current density. Results. The results show that including the anomalous resistivity can reasonably remove the discrepancy between observations and predictions. Meanwhile, the necessary excited level for the ion-acoustic turbulence is tens times of the thermal noise of electrostatic fluctuations in the background plasma, which is an ordinary and low excited level that is easily satisfied. Conclusions. This indicates that the microscopic kinetics of plasma particles possibly play an important and critical role in understanding the dynamics of beam-return current systems in the solar atmosphere and in the physics of solar flares.

Record 209 of 247

EXCITATION OF KINETIC ALFVEN WAVES BY DENSITY STRIATION IN MAGNETO-PLASMAS

Wu, D. J.; Chen, L.


卷: 771; 期: 1; 页: 3-1-3-7

Field-aligned density striation is one of the most common inhomogeneity phenomena in magneto-plasmas, such as in the solar coronal plasma and terrestrial auroral plasma. Kinetic Alfven waves (KAWs) can play an important role in the inhomogeneous heating of coronal magneto-plasmas as well as in the local acceleration of auroral energetic electrons. In this paper, we study the dispersion and instability of KAWs in a magneto-plasma with density striation structures. Results show that KAWs become unstable in the presence of the density striation and the corresponding instability has a maximal growth rate at the perpendicular wavelength close to the spatial scale of the density gradient. Related experimental phenomena in both laboratory and space plasmas are discussed. It is suggested that the excitation of KAWs by the density striation of magneto-plasmas can be of potential importance in understanding the physics of the formation of magneto-plasma filaments and their heating mechanisms, which are often present in the terrestrial auroral plasma, the solar coronal plasma, and other astrophysical plasmas.

Record 210 of 247

Solar type III radio bursts modulated by homochromous Alfven waves

Zhao, G. Q.; Chen, L.; Wu, D. J.


卷: 779; 期: 1; 页: 880-885

Solar type III radio bursts and their production mechanisms have been intensively studied in both theory and observation and are believed to be the most important signatures of electron acceleration in active regions. Recently, Wu et al. proposed that the electron-cyclotron maser emission (ECME) driven by an energetic electron beam could be responsible for producing type III bursts and pointed out that turbulent Alfvén waves can greatly influence the basic process of ECME via the oscillation of these electrons in the wave fields. This paper investigates effects of homochromous Alfvén waves (HAWs) on ECME driven by electron beams. Our results show that the growth rate of the O-mode wave will be


92

significantly modulated by HAWs. We also discuss possible application to the formation of fine structures in type III bursts, such as so-called solar type IIIb radio bursts.

Record 211 of 247

EFFECTS OF ALFVEN WAVES ON ELECTRON CYCLOTRON MASER EMISSION IN CORONAL LOOPS AND SOLAR TYPE I RADIO STORMS

Zhao, G. Q.; Chen, L.; Yan, Y. H.; Wu, D. J.


卷: 770; 期: 1; 页: 75-1-75-9

Solar type I radio storms are long-lived radio emissions from the solar atmosphere. It is believed that these type I storms are produced by energetic electrons trapped within a closed magnetic structure and are characterized by a high ordinary (O) mode polarization. However, the microphysical nature of these emissions is still an open problem. Recently, Wu et al. found that Alfven waves (AWs) can significantly influence the basic physics of wave-particle interactions by modifying the resonant condition. Taking the effects of AWs into account, this work investigates electron cyclotron maser emission driven by power-law energetic electrons with a low-energy cutoff distribution, which are trapped in coronal loops by closed solar magnetic fields. The results show that the emission is dominated by the O mode. It is proposed that this O mode emission may possibly be responsible for solar type I radio storms.

Record 212 of 247

KINETIC ALFVEN TURBULENCE AND PARALLEL ELECTRIC FIELDS IN FLARE LOOPS

Zhao, J. S.; Wu, D. J.; Lu, J. Y.


卷: 767; 期: 2; 页: 109-1-109-5

This study investigates the spectral structure of the kinetic Alfven turbulence in the low-beta plasmas. We consider a strong turbulence resulting from collisions between counterpropagating wavepackets with equal energy. Our results show that (1) the spectra of the magnetic and electric field fluctuations display a transition at the electron inertial length scale, (2) the turbulence cascades mainly toward the magnetic field direction as the cascade scale is smaller than the electron inertial length, and (3)

the parallel electric field increases as the turbulent scale decreases. We also show that the parallel electric field in the solar flare loops can be 10(2)-10(4) times the Dreicer field as the turbulence reaches the electron inertial length scale.

Record 213 of 247

Twist Accumulation And Topology Structure Of A Solar Magnetic Flux Rope

Guo, Y. ;Ding, M. D.;Cheng, X. ; Zhao, J.; Pariat, E.


卷:779;期:2;页: 157(1-13) To study the buildup of a magnetic flux rope before a major flare and coronal mass ejection (CME), we compute the magnetic helicity injection, twist accumulation, and topology structure of the three-dimensional (3D) magnetic field, which is derived by the nonlinear force-free field model. The Extreme-ultraviolet Imaging Telescope on board the Solar and Heliospheric Observatory observed a series of confined flares without any CME before a major flare with a CME at 23: 02 UT on 2005 January 15 in active region NOAA 10720. We derive the vector velocity at eight time points from 18: 27 UT to 22: 20 UT with the differential affine velocity estimator for vector magnetic fields, which were observed by the Digital Vector Magnetograph at Big Bear Solar Observatory. The injected magnetic helicity is computed with the vector magnetic and velocity fields. The helicity injection rate was (-16.47+/-3.52) x 10(40) Mx(2) hr(-1). We find that only about 1.8% of the injected magnetic helicity became the internal helicity of the magnetic flux rope, whose twist increasing rate was -0.18 +/- 0.08 Turns hr(-1). The quasi-separatrix layers (QSLs) of the 3D magnetic field are computed by evaluating the squashing degree, Q. We find that the flux rope was wrapped by QSLs with large Q values, where the magnetic reconnection induced by the continuously injected magnetic helicity further produced the confined flares. We suggest that the flux rope was built up and heated by the magnetic reconnection in the QSLs.


93

Record 214 of 247

On the possibility of spontaneous generation of turbulent Alfven waves in solar plasma by heavy ions (vol 20, 082102, 2013),20,11, 119902(1-1)

Wu, C. S.; Zhao, G. Q.; Chen, L.; Wu, D. J.

PHYSICS OF PLASMAS

卷:20;期:11;页: 119902(1-1)

无

Record 215 of 247

Alfven Waves in the Solar Wind, Chinese Journal of Space Science

Yang L; Chao J K

Chinese Journal of Space Science

卷:33;期:4;页: 353-373 Alfven waves are found to be ubiquitous in the solar wind. Recent progress in observational studies of the waves is reviewed to formulate a microscopic picture for the Alfvenic fluctuations. The main aspects of the observational properties of these waves, including the wave intervals, propagation, evolution, origin and generation, are presented. Then Alfven wave heating and acceleration of the solar wind plasma are briefly introduced. The relation of the waves to rotational and tangential discontinuities, magnetic decreases, and other relatively large-scale structures such as flux tubes/ropes, magnetic clouds and interplanetary coronal mass ejections in the solar wind is particularly investigated. Finally, some remaining open questions are also indicated due to their fundamental importance of understanding of the physical nature of Alfven waves and the role of the waves in heating and accelerating the solar wind.

Record 216of 247

Ion Microprobe Microanalytical Techniques and their Applications in Earth Sciences

Li Qiuli; Yang Wei; Liu Yu; Tang Guoqiang; Hao Jialong; Zhang Jianchao; Hu Sen; Zhao Xuchao;

Chen Yali; Chu Xuelei; Wang Ying; Jiang Yun; Zhang Aicheng; Xu Weibiao; Lin Yangting; Li Xianhua

Bulletin of Mineralogy Petrology and Geochemistry

卷: 32; 期: 3; 页: 310-327

Ion microprobe offers direct microanalyses of element abundances and isotopic compositions at micron to nanometer scales. Along with improving of instrument performance, increasing of instrument number and developing of analytical technique, ion microprobe has gained increasingly wide applications in many aspects of Earth Sciences. This paper presents a brief description of the historical development and the working theory of ion microprobe. We highlight progresses of ion microprobe instrument performance and technique over the past decade, including trace element analysis, stable isotope analysis, isotopic dating and image analysis. We also summarized the major applications and the latest research progresses of ion microprobe in the studies of pre-solar-system materials, the solar nebula evolution, lunar formation and evolution, and early evolution as well as paleoenvironment of the Earth.

Record 217 of 247

Petrography and Mineralogy of the Lunar Regolith Breccia Dhofar 1428

ZHANG, Ai-cheng; XU, Wei-biao

Bulletin of Mineralogy, Petrology and Geochemistry

卷: 32; 期: 2; 页: 222-230

Dhofar 1428 is a lunar meteorite from Oman.Our investigations reveal that Dhofar 1428 is a regolith breccia dominated by highlands ferroan anorthositic components.Petrographic texture of pyroxene in the spinel-bearing lithic clast indicates that some magnesian anorthosites were derived from assimilation of anorthositic crust during the ascending of magma from the deep crust of the Moon.Magnesium-rich feature and Fe-Mn trend of olivine,relict barred-olivine texture,and the presence of troilite along the margin of the spherule clast indicate that it was derived from chondrite,rather than formed by melting and recrystallization of rocks on the lunar surface.In addition,we suggest that the different Fe-Mn trends between high-Fe pyroxenes and low-Fe pyroxenes are probably due to various preferences of Mn and Fe2+ for the M2 site in the

Laboratory for Astrochemistry and

Planetary Sciences


94

pyroxene crystal structure.

Record 218 of 247

The water content and parental magma of the second chassignite NWA 2737: Clues from trapped melt inclusions in olivine

He, Qi; Xiao, Long; Hsu, Weibiao; Balta, J. Brian; McSween, Harry Y.; Liu, Yang

METEORITICS & PLANETARY SCIENCE

卷: 48; 期: 3; 页: 474-492

NWA 2737, the second known chassignite, mainly consists of cumulate olivine crystals of homogeneous composition (Fo=78.7 +/- 0.9). These brown colored olivine grains exhibit two sets of perpendicular planar defects due to shock. Two forms of trapped liquids, interstitial melts and magmatic inclusions, have been examined. Mineral assemblages within the olivine-hosted magmatic inclusions include low-Ca pyroxene, augite, kaersutite, fluorapatite, biotite, chromite, sulfide, and feldspathic glass. The reconstructed parental magma composition (A#) of the NWA 2737 is basaltic and resembles both the experimentally constrained parental melt composition of chassiginites and the Gusev basalt Humphrey, albeit with lower Al contents. A# also broadly resembles the average of shergottite parent magmas or LAR 06319. However, we suggest that the mantle source for the chassignite parental magmas was distinct from that of the shergottite meteorites, particularly in CaO/Al2O3 ratio. In addition, based on the analysis of the volatile contents of kaersutite, we derived a water content of 0.480.67 wt% for the parental melt. Finally, our MELTS calculations suggest that moderate pressure (approximately 6.8kb) came closest to reproducing the crystallized melt-inclusion assemblages.

Record 219 of 247

Record of S-rich vapors on asteroid 4 Vesta: Sulfurization in the Northwest Africa 2339 eucrite

Zhang, Ai-Cheng; Wang, Ru-Cheng; Hsu, Wei-Biao; Bartoschewitz, Rainer

GEOCHIMICA ET COSMOCHIMICA ACTA

卷: 109; 页: 1-13

In the Northwest Africa (NWA) 2339 eucrite, a few high-Fe pigeonite fragments were partially replaced by fine-grained troilite, Mg-rich augite, silica, with minor ilmenite and Mg-rich ferrosilite.

The relict pigeonite has distinctly lower Fe/Mn values (17-18) than those (similar to 30) of augite and Mg-rich ferrosilite in the fine-grained replacement textures and other eucritic pyroxenes in NWA 2339. The few plagioclase grains associated with these Fe-rich pigeonite fragments contain high albite components (Ab(17-31)). Similar replacement textures are also present in a lithic clast consisting of pyroxene and Na-rich plagioclase (Ab(20-25)). In this lithic clast, high-Fe subcalcic augite was replaced by troilite, Mg-rich hedenbergite, silica, and minor ilmenite whereas Mg-rich pigeonite remains intact. Troilite also occurs as tiny inclusions in porous regions of plagioclase. Moreover, the porous regions of plagioclase are enriched in Si and depleted in Al, Ca, and Na, compared to relict plagioclase. These textures indicate that the formation of troilite-rich mineral assemblages is related to the reaction between FeSiO3 component in pyroxene and S-rich vapors; whereas, the formation of tiny troilite in porous regions of plagioclase is related to the reaction between Fe2+ in plagioclase and S-rich vapors. X-ray mapping results reveal that during sulfurization of pyroxene and plagioclase, lithophile elements Mn, Al, Ca, Na, and Mg were removed to various extents, very likely by the S-rich vapors. Based on our observations, the S-rich vapors could be dry S-O-P vapors, which most likely have been formed by volatilization of pre-existing S, P-bearing materials due to impact heating on the surface of asteroid 4 Vesta. (C) 2013 Elsevier Ltd. All rights reserved.

Record 220 of 247

Oxygen isotope compositions of Al-rich chondrules from carbonaceous chondrites

WANG, Ying; HSU, W.; LI, X.; LI, Q.

Mineralogical Magazine

卷: 77; 期: 1; 页: 2462

Al-rich chondrules (ARCs) are rare objects with >10 wt% bulk Al2O3 content. They have petrological, chemical, and oxygen isotopic characteristics intermediate between Ca,Alrich inclusions (CAIs) and ferromagnesian chondrules (FMCs) [1]. ARCs are an unique window to study the orgins of CAIs and chondrules and their genetic relationship.


95

Record 221 of 247

SIMS dating of eucritic zircons

Hsu, W.; Wang, L.; Zhang, A.

76th Annual Meeting of the Meteoritical Society

卷: 48; 页: A172

Eucrites are the oldest basalts formed at the very beginning of the solar system. They recorded early differ-entiation and volcanism on a small planetary body, probably 4 Vesta. In-depth investigations revealed that eucrites had experi-enced varying degrees of post-thermal, shock, and aqueous al-terations [1-3]. To better constrain the timing of magmatic evo-lution and post-thermal history on 4 Vesta, we carried out in situ dating of zircon and baddeleyite found in three eucrites. The primary goal of this study is to seek the evidence of disturbance on eucrite crystallization ages due to secondary metamorphisms.

Record 222 of 247

Youxi, a newly found mesosiderite from China

Hsu, W.; Wang, L.

METEORITICS & PLANETARY SCIENCE

卷: 48; 页: A171

The Youxi mesosiderite was found in 2006 at a construction site in Youxi county, Sanming city, Fujian Province of China. It weighs 218 kg and remains relatively fresh. The fusion crust is still visible (Fig. 1). We carried out a preliminary study on its petrology and mineralogy and found that Youxi is a Type 2A mesosiderite.

Record 223 of 247

富集型玄武质火星陨石 NWA 2975 的岩石学和

稀土元素地球化学特征

何琦; 肖龙; 徐伟彪

中国矿物岩石地球化学学会第 14 届学术年会

卷: 19; 页: 611-612

NWA 2975 火星陨石是一个玄武质的 S-类火星陨

石，于 2005 年被发现于摩洛哥或阿尔及利亚。

前人的研究反映了火星陨石 NWA 2975 也是一

种富集型的玄武质 S-类火星陨石，与 Shergotty

和 Los Angeles 等相似。本文的研究将在岩相学

的基础上，对该陨石中的主要矿物进行原位的主

量和微量元素的分析,用以探讨该火星陨石的分

异演……

Record 224 of 247

灶神星表面流体-岩石相互作用的陨石学记录

张爱铖; 王汝成; 徐伟彪


卷: 19; 页: 628-629

类地行星和小行星表面是否存在流体、流体的成

分是什么及流体如何影响类地行星和小行星表

面岩石的矿物和地球化学特征一直是行星科学

研究最重要的内容之一。灶神星是最近小行星深

空探测最重要的对象之一，美国 DAWN 计划的

初步探测结果表明灶神星表面可能存在着水冰，

但这些水冰如何影响灶神星表面岩石仍……

Record 225 of 247

新近发现的罗布泊陨石

李少林; 徐伟彪


卷: 19; 页: 613-614

2012 年 11 月，中国陨石网发起人赵志强随同罗

布泊野人俱乐部的武宗云、刘福英、和刘生，深

入新疆罗布泊区域，开展了一次为期 21 天的猎

陨活动，发现和收集了 13 块陨石样品。随着越

来越多陨石的发现,新疆沙漠地区日渐成为我国

陨石的主要富集地之一。本文报道了该 13 块陨

石的矿物岩石学特征。

Record 226 of 247

Water content and chlorine isotope composition of the moon

WANG, Ying; GUAN, Yunbin; XU, Weibiao; Eiler, J. M.

第十届全国同位素地质年代学与同位素地球化

学学术讨论会论文集

期: 1; 页: 1

从上世纪 60 年代末到本世纪初的几十年里，月

球一直被认为相对于地球严重亏损挥发性元素。

据 Taylor 等人估计，月球含水量不足 1ppb，比

地球和火星低至少 6 个数量级。最近几年，利用

先进的二次离子质谱仪（SIMS）和红外光谱仪

（FTIR），研究者在月球火山玻璃、磷灰石、斜

长石和橄榄石中的熔体包裹体内检测到了几个

至几千 ppm 的水。


96

Record 227 of 247

Ion microprobe dating of zircon and baddeleyite from eucrites

WANG, Ying; WANG, Linyan; ZHANG, Aicheng; XU, Weibiao

中国极地科学年会论文集

期: 1; 页: 1

钙长辉长无球粒陨石（Eucrite）与奥长古铜无球

粒陨石（Diogenite）和钙长紫苏无球粒陨石

（Howdite）具有相似的化学成分和同位素组成，

因而统称为 HED 陨石。反射光谱和理论模型计

算等表明，4 号小行星灶神星（Vesta）是 HED

陨石最可能的母体。……

Record 228 of 247

Observation Plan for Refining Shape Model of (6) HEBE

Lu, Xiaoping; Zhao, Haibin; You, Zhong

EARTH MOON AND PLANETS

卷: 110; 页: 81-89

As the number of observatories located on the surface of Earth is increasing largely in decades more and more photometric data of asteroids is observed to make the research about their various physical and chemical characteristics. Compared with hundreds of thousands of asteroids found up to now, rare hundreds of three-dimensional shape models of asteroids have been built from the tremendous photometric data with incessant observations, i.e. lightcurves. For some specific asteroid already with many observed lightcurves, the unceasing observation is not too much valuable, nevertheless an additional lightcurve observed in a request viewing aspect can refine the shape model and other related parameters. This article taking the asteroid (6) HEBE for example, attempts to introduce a method to make the observation plan by combining the request of the shape model and the orbital limitation of asteroids. Through analyzing the distribution of lightcurves of (6) HEBE, small cabins without any lightcurve data are found, which can be filled by new observations at some specified dates when the positions of Asteroid, Sun, Earth are limited as the request

geometry.

Record 229 of 247

A fast ellipsoid model for asteroids inverted from lightcurves

Lu, Xiao-Ping; Zhao, Hai-Bin; You, Zhong


卷: 13; 期: 4; 页: 471-478

Research about asteroids has recently attracted more and more attention, especially focusing on their physical structures, such as their spin axis, rotation period and shape. The long distance between observers on Earth and asteroids makes it impossible to directly calculate the shape and other parameters of asteroids, with the exception of Near Earth Asteroids and others that have passed by some space-crafts. Photometric measurements are still generally the main way to obtain research data on asteroids, i.e. the lightcurves recording the brightness and positions of asteroids. Supposing that the shape of the asteroid is a triaxial ellipsoid with a stable spin, a new method is presented in this article to reconstruct the shape models of asteroids from the lightcurves, together with other physical parameters. By applying a special curvature function, the method calculates the brightness integration on a unit sphere and Lebedev quadrature is employed for the discretization. Finally, the method searches for the optimal solution by the Levenberg-Marquardt algorithm to minimize the residual of the brightness. By adopting this method, not only can related physical parameters of asteroids be obtained at a reasonable accuracy, but also a simple shape model of an ellipsoid can be generated for reconstructing a more sophisticated shape model.

Record 230 of 247

Atmospheric extinction coefficients and night sky brightness at the Xuyi Observation Station

Zhang, Hui-Hua; Liu, Xiao-Wei; Yuan, Hai-Bo; Zhao, Hai-Bin; Yao, Jin-Sheng; Zhang, Hua-Wei; Xiang, Mao-Sheng


卷: 13; 期: 4; 页: 490-500

We present measurements of the optical broadband atmospheric extinction coefficients and the night sky brightness at the Xuyi Observation Station of Purple Mountain

Xuyi Observation Station


97

Observatory. The measurements are based on CCD imaging data taken in the Sloan Digital Sky Survey's g, r and i bands with the Xuyi 1.04/1.20m Schmidt Telescope for the Xuyi Schmidt Telescope Photometric Survey of the Galactic Anti-center (XSTPS-GAC), the photometric part of the Digital Sky Survey of the Galactic Anti-center (DSS-GAC). The data were collected during more than 140 winter nights from 2009 to 2011. We find that the atmospheric extinction coefficients for the g, r and i bands are 0.69, 0.55 and 0.38 mag/airmass, respectively, based on observations taken on several photometric nights. The night sky brightness determined from images with good quality has median values of 21.7, 20.8 and 20.0 mag arcsec(-2) and reaches 22.1, 21.2 and 20.4 mag arcsec(-2) under the best observing conditions for the g, r and i bands, respectively. The relatively large extinction coefficients compared with other good astronomical observing sites are mainly due to the relatively low elevation (i.e. 180 m) and high humidity at the station.

Record 231 of 247

Photometric Observation of 1542 Schalen

Li, Bin; Zhao, Haibin; Han, Xianming L.; Klinglesmith, Daniel A., III; Hanowell, Jesse

Minor Planet Bulletin

卷: 40; 期: 2; 页: 68-69

CCD photometric observations of asteroid 1542 Schalen over ten nights in 2012 October and November were used to determine a synodic rotation period of 7.516 Â± 0.002 h and an amplitude of 0.49 ± 0.02 mag.

Record 232 of 247

Lightcurve Analysis of Four Asteroids

Li, Bin; Zhao, Haibin; Han, Xianming L.; Annable, Lina R.; Finkel, Eli M.; Heffner, Orry R.; Kidd, Adam W.; Magnetta, Bradley J.; Ramires, Tiffany M.; Rastede, Frederick W.; Sproston, Sean G.


卷: 40; 期: 2; 页: 62-63

From June 2011 through May 2012 May, photometric data for four asteroids were obtained using the Southeastern Association for Research in Astronomy (SARA) telescope located at the Kitt Peak National Observatory. The following synodic periods were found: 4808 Ballaero, P = 8.8976 Â±

0.0007 h; 7750 McEwen, P = 27.82 ± 0.01 h; 11941 Archinal, P = 2.717 Â±0.006 h; and (47035) 1998WS, P = 7.996 ± 0.001 h.

Record 233 of 247

Photometric Observation of 3024 Hainan, 3920 Aubignan, and 5951 Alicemonet

Li, Bin; Zhao, Haibin; Hand, Xianming L.; Liu, Wenjuan; Sun, Luming; Shi, Jingjing; Gao, Shan, Zhou, Hongyan


卷: 40; 期: 1; 页: 43-44

Three minor planets were measured photometrically between 2012 September 4 and 21 using the SARA (Southeastern Association for Research in Astronomy) South telescope, located in Cerro Tololo Inter-American Observatory. The following synodic periods were found: 3024 Hainan, P = 11.785 Â± 0.005 h; 3920 Aubignan, P = 4.4762 Â± 0.0005 h; and 5951 Alicemonet, P = 3.8871 Â± 0.0005 h.

Record 234 of 247

嫦娥二号卫星多目标多任务设计与经验

孟林智; 黄江川; 叶培建; 张廷新; 饶炜; 乔栋;

李春来; 麻永平; 姜晓军; 季江徽

中国科学:技术科学

卷: 43; 期: 6; 页: 585-595

嫦娥二号卫星在圆满完成后续工程先导技术验

证和科学探测任务后，又相继开展了日-地拉格

朗日 L2 点和飞越 Toutatis 小行星探测，开创了

我国多目标探测的先河，开拓了拉格朗日点和小

天体新的探测领域。在剖析以往国际上典型多目

标多任务探测器特点后，本文紧扣牵引技术发展

主题，提出了以系统创新拓展领域,提升能力，

带动技术突破和产品发展的思路，设计了在短周

期等约束条件下实现多目标探测的策略与步骤；

其次针对设定目标任务和推进技术发展的需求，

提出了实现更远距离、更多技术验证的高可靠、

高精度和自主运行的设计要点，简述了相关技术

突破的情况；基于在轨运行表现，分析、汇总嫦

Laboratory for Planetary Science and

Deep Space Exploration


98

娥二号的实现结果和预期改进目标；最后，梳理

总结了嫦娥二号在任务设计、技术突破和实施程

序与方法等方面的成功创新经验，可供未来任务

借鉴。

Record 235 of 247

Tidal Evolution of the Kepler Candidate Two-planet Systems

Dong, Yao; Ji, JiangHui

Acta Astronomica Sinic

卷: 54; 期: 4; 页: 350-361

The tidal evolution of ten Kepler candidate two-planet systems is investigated by using the general secular theory, and then a general picture of the tidal evolution for these systems is described. Furthermore, the theoretical results of KOI 1239 system show that the dissipation part of the tidal effect acts as a dominant factor, which may cause the eccentricity to decrease in the tidal evolution. However, the conservative part of the planetary tide and the relativistic effects may damp the excitation of the eccentricity of the inner planet with the outer planet’s perturbation. Both the initial eccentricity of the outer planet and the tidal dissipation factors can also affect the tidal evolution. In addition, the numerical simulations are extensively carried out to investigate the tidal evolution of KOI 1239 system, and the numerical outcomes are well consistent with those of the general secular theory.

Record 236 of 247

A Study on the Characteristics of the Structure of Vega's Debris Disk

LU, Tao; Ji, JiangHui


卷: 54; 期: 2; 页: 131-146

Clumpy structure in the Vega’s debris disk has been previously reported at millimeter wavelengths and attributed to the concentrations of dust grains trapped in resonances with a potential planet. However, current imaging at multi-wavelengths with higher sensitivity is against the former observed structure. The disk is now revealed to have a smooth structure. A planet orbiting Vega could not be neglected, but the present-day observations may place a severe constraint on the orbital parameters for the potential planet. Herein, we utilize modified MERCURY codes to numerically simulate Vega

system, consisting of debris disk and a planet. In our simulations, the initial inner and outer boundaries of the debris disk are assumed to be 80 AU and 120 AU, respedtively. The radius of dust grains distributes in the range from 10 μm to 100 μm, in nearly coplanar orbits. From the outcomes, we show that the evolution of debris disk is consistent with recent observations, if there is no planet orbiting Vega. However, if Vega owns a planet with a high eccentricity (e.g., e=0.6), the planetary semi-major axis cannot be larger than 60 AU, otherwise, the structure of debris disk will congregate due to the existence of the postulated planet. The 2:1 mean motion resonances may play a significant role in sculpting the debris disk.

Record 237 of 247

The Review of Thermal Models for Asteroids

Yu, Liangliang; Ji, Jianghui

Progress in Astronomy

卷: 31; 期: 2; 页: 185-201

In this paper, several typical thermal models for asteroids, which are widely applied in the asteroid science in recent years, are extensively reviewed. The fundamental physics and application of these models are extensively discussed. In general, the thermal models of asteroids can be divided into two categories: the Simplified Model and Thermal-Physical Model, the former is always used to estimate the asteroids albedo and diameter, while the latter adopts detailed shape model and classic thermal laws of physics as realistically as possible to simulate complex thermal environment of the asteroid surface. Through the numerical process of thermal model, the temperature distribution of the asteroid surface can be obtained and its thermal infrared radiation can be calculated, which can be used to fit the mid-IR observations of the asteroid so as to determine its effective diameter, albedo, and thermal inertia. Furthermore, an appropriate simulation of an asteroids surface thermal environment from a thermal model does great benefits to study the thermal history of the asteroid and other related procedures such as Yarkovsky and YORP effects.


99

Record 238 of 247

嫦娥二号飞越小行星试验中图塔蒂斯轨道确定

与精度分析

胡寿村; 季江徽; 赵玉晖; 孟林智

Scientia Sinica Technologica

卷: 43; 期: 5; 页: 506-511

本文利用兴隆、盱眙观测站及夏威夷大学、智利

CTIO 天文台在 2012 年 5~11 月获得的 300 多组

观测数据,以及历史光学测角与雷达测距测速资

料,构建动力学模型对 4179 号小行星图塔蒂斯

(Toutatis)进行轨道确定,获得的小行星定轨内符

合精度优于 5km。本文给出了在飞越时刻(北京

时间 2012 年 12 月 13 日 16:30)的图塔蒂斯轨道

参数,并对小行星定轨精度进行分析,定轨结果被

嫦娥二号飞越小行星试验任务正式采用,实现其

首次对图塔蒂斯的近距离飞越探测,交会距离小

于 3.2km。

Record 239 of 247

Error Analysis and Trajectory Correction Maneuvers of Lunar Transfer Orbit

ZHAO, Yuhui; HOU, Xiyun; LIU, Lin


卷: 54; 期: 3; 页: 261-273

For the sample return lunar missions and human lunar exploration, this paper studies the characteristics of both the Earth-Moon transfer orbit and the return orbit. On the basis of the error propagation matrix, the linear equation to estimate the first midcourse trajectory correction maneuver (TCM) is figured out. Numerical simulations are performed, and the features of error propagation in lunar transfer orbit are given. The advantages, disadvantages, and applications of two TCM strategies are discussed, and the computation of the second TCM of the return orbit is also simulated under the conditions at the reentry time.

Record 240 of 247

A Research on Imaging Strategy and Imaging Simulation of Toutatis in the Chang'e 2 Flyby Mission

ZHAO, Yuhui; WANG, Su; HU, Shoucun; JI, Jianghui


卷: 54; 期: 5; 页: 447-454

For the flyby mission of Toutatis by the Chang’e 2 detector, the light conditions for imaging are

calculated in this paper based on the orbital parameters of both the detector and the asteroid and the viewing angle. On the basis of the result, it’s suggested to take the picture during the out-bound track, and the proposed orientation for the optical axis in the mean equator and equinox of J2000.0 coordinate system is represented to be

(118.02º, 22.03º). Based on the shape model determined by radar data, the Oren-Nayar reflection model is used for imaging simulation

according to the position relation among the sun，

the asteroid, and the detector．The simulations are done at the distances of 300 km 500 km, and 1000 km respectively from the asteroid after flyby, and the results are certificated by the optical images obtained in the mission.

Record 241 of 247

On Nominal Formation Flying Orbit with a Small Solar System Body

Zhao, Yuhui; Hu, Shoucun; Hou, Xiyun; Liu, Lin

Lecture Notes in Electrical Engineering

卷: 187; 期: 26; 页: 391-399

It is very difficult for an explorer to orbit a low-mass and irregularly shaped small body in the solar system. In this case, formation flying with the small body is a workable solution. This paper discusses two strategies of formation flying based on two different dynamic models. The orbit resulted from the C–W equation and the halo orbit around libration point L1 in the Circular Restricted Three-body Problem (CRTBP) are considered as nominal orbit respectively. Numerical simulation indicates the effect of the magnitude of μ on the stability and other features of the halo orbits, where μ is a parameter weighing the gravity of the small body. The result shows that the CRTBP is more fuel-saving and therefore a more appropriate dynamic model for solving the formation flying problem. This paper also works out a dynamic model involving solar radiation pressure. Simulation result shows that, in this condition, the C–W equation has no significant advantage.

Record 242 of 247

POSSIBLE TRANSIT TIMING VARIATIONS OF THE TrES-3 PLANETARY SYSTEM

Jiang, Ing-Guey; Yeh, Li-Chin; Thakur, Parijat; Wu, Yu-Ting; Chien, Ping; Lin, Yi-Ling; Chen, Hong-Yu; Hu, Juei-Hwa; Sun, Zhao; Ji, Jianghui


100


卷: 145; 期: 3; 页: 68-1-68-8

Five newly observed transit light curves of the TrES-3 planetary system are presented. Together with other light-curve data from the literature, 23 transit light curves in total, which cover an overall timescale of 911 epochs, have been analyzed through a standard procedure. From these observational data, the system's orbital parameters are determined and possible transit timing variations (TTVs) are investigated. Given that a null TTV produces a fit with reduced chi(2) = 1.52, our results agree with previous work, that TTVs might not exist in these data. However, a one-frequency oscillating TTV model, giving a fit with a reduced chi(2) = 0.93, does possess a statistically higher probability. It is thus concluded that future observations and dynamical simulations for this planetary system will be very important.

Record 243 of 247

Tidal evolution of the Kepler-10 system

Dong, Yao; Ji, Jianghui


卷: 430; 期: 2; 页: 951-960

We investigate by numerical methods the tidal evolution of the Kepler-10 system, which consists of an inner rocky planet and an outer terrestrial planet, by considering various initial eccentricity pairs that follow conservation of angular momentum of the system. Our results cover the range of all reasonable initial eccentricities with various mass ratios of the two planets for the Kepler-10 system; all initial eccentricity pairs can produce the present observed orbits within certain errors. Additional simulations with alternate values of dissipation factor Q(1)' are carried out, where the results may be indicative of the possible range 50 <= Q(1)' <= 500. Moreover, considering the density of the terrestrial planets and the previous models, we provide a possible constraint on the mass of Kepler-10c of 7M(circle plus) <= m(2) <= 20M(circle plus). Finally, we propose a possible planetary formation scenario for the Kepler-10 system: both planets may form from a distant region in the disc, then the inner planet may experience planet-planet scattering, following as tidal decay and circulation. However, the outer companion may undergo mainly disc migration, judging from our model.

Record 244 of 247

Establish and use of the numerical ephmerides for Near-Earth Asteroids

HU, Shoucun; ZHAO, Yuhui; JI, Jianghui

第二届航天飞行动力学技术研讨会论文集

期: 1; 页: 1

为配合我国未来近地小行星深空探测的需要，本

文针对建立近地小行星数值历表中的若干问题

进行了探讨，分析了近地小行星的受摄运动模型，

在此基础上给出了建立小行星数值历表的一般

方法和流程，并针对目前所发现的 9941 颗近地

小行星初步建立了适用于 50 年内的数值历表库，

结果表明该历表的拟合精度和计算速度均满足

小行星深空探测轨道设计的要求。

Record 245 of 247

Using finite element definitions to compute the gravitation of Toutatis

ZHAO, Yuhui; WANG, Su; JI, Jianghui

中国宇航学会深空探测技术专业委员会第九届

学术年会论文集

期: 9; 页: 111-116

针对太阳系小天体形状不规则、密度不均匀等特

点，文章采用体积离散方法计算小天体引力场球

谐系数和表面重力场分布情况，以(433)Eros 为

例验证该方法的可靠性，并使用该方法对我国小

行星探测任务拟探测的 1996 FG3 小行星的重力

场进行了计算。文章以嫦娥二号探测器飞越的图

塔蒂斯小行星为例，结合相应的雷达观测数据提

供的小行星形状模型，计算其表面引力势情况，

为通过飞越任务获取的光学图像分析其表壤的

分布、流向等提供了相应的理论依据。

Record 246 of 247

The Ginger-shaped Asteroid 4179 Toutatis: New Observations from a Successful Flyby of Chang'e-2

Huang, J; Ji, J; Ye, P; Wang, X; Yan, J; Meng, L; Wang, S; Li, C; Li, Y; Qiao, D; Zhao, W; Zhao, Y; Zhang, T; Liu, P; Jiang, Y; Rao, W; Li, S; Huang, C; Ip WH; Hu, S; Zhu, M; Yu, L; Zou, Y; Tang, X; Li, J; Zhao, H; Huang, H; Jiang, X; Bai, J

Scientific Reports

卷: 3; 期: 1; 页: 3411-3416

On 13 December 2012, Chang'e-2 conducted a successful flyby of the near-Earth asteroid 4179


101

Toutatis at a closest distance of 770 ± 120 meters from the asteroid's surface. The highest-resolution image, with a resolution of better than 3 meters, reveals new discoveries on the asteroid, e.g., a giant basin at the big end, a sharply perpendicular silhouette near the neck region, and direct evidence of boulders and regolith, which suggests that Toutatis may bear a rubble-pile structure. Toutatis' maximum physical length and width are (4.75 × 1.95 km) ±10%, respectively, and the direction of the +z axis is estimated to be (250 ± 5°, 63 ± 5°) with respect to the J2000 ecliptic coordinate system. The bifurcated configuration is indicative of a contact binary origin for Toutatis, which is composed of two lobes (head and body). Chang'e-2 observations have significantly improved our understanding of the characteristics, formation, and evolution of asteroids in general.

Record 247 of 247

Investigation of Thermal Inertia and Surface Properties for Near-earth Asteroid (162173) 1999 JU3

Yu Liangliang; Ji Jianghui; Wang Su


卷:54;期:6;页:537-549

In order to obtain the substantial information about the physical and thermal properties of target asteroid (162173) 1999 JU3, which will be visited by Hayabusa 2 in a sample return mission, we estimate a possible thermal inertia distribution over its surface, and infer the major material component on it. In addition, the effective diameter and geometric albedo are derived, to be about D_(eff)= 1.130.03 km, rho_v = 0.0420.003, respectively. Moreover, the average thermal inertia is evaluated to be about (30050) J·m~(-2)·s~(-0.5)·K~(-1). As a result, a global thermal inertia distribution is assumed to describe the situation on the asteroid's surface. According to the outcomes derived with such a distribution, we infer that the major area over the surface of the proposed target may be covered by loose materials, such as rocky debris, sand, and so on, but few bare rocks may exist in a very small region. In this sense, it is feasible for Hayabusa 2 to probe the proposed target, which will certainly bring back significant scientific outcomes after the successful sample return mission.


102

紫台历年发表论文情况

专利

序

号类型名称发明人专利号状态

1 发明专利利用光学摄像装置制作分形图案的方

法与制作分形动画的方法刘四明 201310049839.X 申请

2 发明专利液氦和液氮温区的 C 波段隔离器及应

用刘洁,单文磊 201310069089.2 申请

3 发明专利一种 OTF 观测扫描方法孙继先,杨戟,逯

登荣 201310251925.9 申请

4 发明专利大视场天文望远镜主镜轴向和侧支撑

自动优化设计方法

杨戟,王海仁,程

景全,娄铮,郑宪

忠,钱元

201310662642.3 申请

5 发明专利天文望远镜 CCD 相机的大口径卷帘式

快门

姚大志,刘伟,华

园园 201310549759.0 申请

6 发明专利波导型集成多路功率分配器单文磊 ZL 201010509692.4 授权

7 发明专利射电望远镜的副面的自适应调焦方法杨戟,孙继先,逯

登荣,李阳 ZL 200910264228.0 授权

8 发明专利射电望远镜的副面的主动控制方法杨戟,孙继先,李

阳 ZL 200910032452.7 授权

9 发明专利暗弱空间碎片高精度定位方法鲁春林,张晓祥 ZL 201110368826.X 授权

10 发明专利空间碎片身份识别方法熊建宁,赵长印 ZL 201110367652.5 授权

11 发明专利快速星图匹配方法张晓祥,高昕 ZL 201110361108.X 授权

122 122 132

155

82

111 116

140

98

73

104

72

49 61

80 82

0

20

40

60

80

100

120

140

160

180

2006年 2007年 2008年 2009年 2010年 2011年 2012年 2013年

篇数

年度

第一单位论文

第一单位SCI论文


103

2013 年度发表科研论文、专著、专利一览表

团组与学科片论文

总数

第一

单位

论文

SCI

论文

第一

单位SCI

论文

国际

合作

论文

专利

申请

专利

授权

宇宙学、暗物质及高能天体物理研究 4 1 4 1 0 0 0

宇宙伽玛暴、中子星及相关物理研究 6 4 5 3 3 0 0

太阳高能及相关物理过程研究 16 11 12 8 11 1 0

太阳活动的多波段观测研究 15 9 14 9 6 0 0

暗物质和空间天文实验室 23 11 18 9 9 0 0

暗物质和空间天文合计 64 36 53 30 29 1 0

恒星结构、演化和脉动研究 6 4 2 1 1 0 0

南极天文中心 27 10 23 7 15 0 0

星系宇宙学和暗能量研究 3 2 3 2 3 0 0

星系中的恒星形成研究 19 6 14 4 15 0 0

分子云与恒星形成研究 28 14 22 10 23 1 1

毫米波和亚毫米波技术实验室 10 4 9 4 4 1 2

青海观测站 6 2 5 1 4 1 0

南极天文和射电天文合计 99 42 78 29 65 3 3

空间目标与碎片观测研究中心 23 22 6 6 0 0 3

卫星精密定轨及应用研究 0 0 0 0 0 0 0

CCD 相机研制实验室 0 0 0 0 0 1 0

应用天体力学和空间目标与碎片合计 23 22 6 6 0 1 3

近地天体探测和太阳系天体研究 1 0 1 0 1 0 0

历算和天文参考系研究 12 8 7 3 1 0 0

太阳和太阳系等离子体研究 16 14 12 10 4 0 0

天体化学和行星科学实验室 12 6 5 3 2 0 0

盱眙观测站 6 3 3 0 0 0 0

行星科学与深空探测实验室（筹） 14 9 3 1 2 0 0

行星科学和深空探测合计 61 40 31 17 10 0 0

总计 247 140 168 82 104 5 6


104

紫台主要科研项目统计

2013 年度在研科研项目

项目类型在研项目

总数占比

当年新开

项目数

在研项目当年

到账经费/万

国家任务 153 59% 65 6009

中科院任务 70 27% 24 4991

研究所自选 3 1% 1 25

横向委托 16 6% 6 394

地方任务 15 6% 1 112

其他 2 1% 0 0

总和 259 100% 97 11531

0

50

100

150

200

250

300

2006 2007 2008 2009 2010 2011 2012 2013

50 60

90

117 137

170

240 259

项目数

年度


105

学术报告

序号

日期报告人单位职称题目

1 2013/1/11 杨浩华中师范大学天体物理

研究所博士 Magnetic Fields of Young

Stars

2 2013/1/18 Martin Lemoine 法国天体物理研究所教授

The microphysics of particle

acceleration at relativistic

shock wave and some

consequences

3 2013/3/8 郭新（Sun Kwok）香港大学教授

Synthesis of Organic

Compounds in the Late

Stages of Stellar

4 2013/3/21 Kathy Reeve Harvard-Smithsonian

Center for Astrophysics 博士

Energy diagnostics, current

sheet formation and

X-ray/EUV emission in

thermodynamic MHD CME

simulations

5 2013/3/15 刘继峰国家天文台研究员 Black holes in the Milky

Way and nearby galaxies

6 2013/4/3 Xiaoying Xu Carnegie Mellon

University 博士

Anistropic analyses of

baryon acoustic oscillation

7 2013/5/7 Li Zeng 哈佛大学天文系博士 Planetary Interiors Come

Alive

8 2013/4/17 刘忠云南天文台研究员抚仙湖一米红外望远镜数

据的使用和研究进展

9 2013/5/13 Masaru Matsuoka JAXA, Riken, Japan 研究员 Highlights of MAXI results

10 2013/6/4 康熙紫金山天文台研究员

An alternative way to

constrain the nature of the

Warm Dark Matter

11 2013/6/8 Thomas Greve Univ. College London 教授

Overcoming nightmares to

reach your dream -

submillimetre stacking of z >

3 UV-selected galaxies

12 2013/9/30 Michael Busch

National Radio

Astronomy Observatory

& SETI Institute 博士后

Spin, Shape, and Interior of

Near-Earth Asteroid 4179

Toutatis

13 2013/6/21 Christian Henkel Max-Planck-Institut für

Radioastronomie 博士

New Masers, Physical

Constants, Densities and

Temperatures: From

Effelsberg to ALMA

14 2013/6/27 Willem Baan the Netherlands Institute

for Radio Astronomy 博士

The ISM of ULIRGs,

Starbursts and the Galaxy:

masers and molecules

15 2013/7/4 Bronfman Leonardo Chile University 教授 R&D of mm/submm-wave

instruments in PMO

16 2013/7/23 秦胜利德国科隆大学博士大质量恒星形成区的亚毫

米/远红外分子线观测

17 2013/8/8 Fulai GUO Swiss Federal Institute of

Technology

Zwicky奖

学者

Growth and Feedback of

Supermassive Black Holes in

Galaxies and Galaxy

Clusters

18 2013/8/15 Wei Xue INFN/SISSA, Italy 博士 Fermi Bubble Under Dark

Matter Scrutiny

19 2013/9/5 Yingna Su Harvard-Smithsonian

Center for Astrophysics 研究员

Observations and Modeling

of Solar Eruptions

20 2013/9/4 黄狮勇武汉大学电子信息学院博士日地空间等离子体中湍流


106

序号

日期报告人单位职称题目

的观测研究

21 2013/9/11 David Coward University of Western

Australia 教授

Coincident gravitational

wave and optical detections

of neutron star mergers:

strategies for the future

22 2013/9/11 David Coward University of Western

Australia 教授

The UWA Zadko Telescope:

current and future science

and collaborations

23 2013/9/23 Jingwen Wu University of California,

Los Angeles 博士

WISE Hot DOGs: The most

Luminous Galaxies in the

Universe

24 2013/9/18 Alain Omont Institut Astrophysique de

Paris 教授

H2O emission in Herschel

high-z sub-millimetre

galaxies

25 2013/9/30 Michael Busch

National Radio

Astronomy Observatory

& SETI Institute 博士后

Spin, Shape, and Interior of

Near-Earth Asteroid 4179

Toutatis

26 2013/11/25 Lingzhen Zeng Harvard-Smithsonian

Center for Astrophysics Physicist

The Cosmology Large

Angular Scale Surveyor

(CLASS)

27 2013/10/18 李晓卿南京师范大学教授

Kinetics of massive

gravitons as a dark matter

and dark energy

28 2013/11/27 Fulvio Melia 美国亚利桑那大学教授 The Galactic Supermassive

Black Hole

29 2013/11/18 田晖美国哈佛-史密松天体物

理中心博士

IRIS 卫星的仪器运营与科

学数据

30 2013/11/20 Zimovets, A.

Struminsky

俄罗斯科学院空间研究

所教授

Solar and Heliosphere

Physics aboard the

INTERHELIO-PROBE

mission

31 2013/11/20 Zimovets, A.

Struminsky

俄罗斯科学院空间研究

所教授

Spectral analysis of coronal

and chromospheric hard

X-ray sources in a partially

occulted solar flare observed

by the RHESSI and HEND

onboard 2001 Mars Odyssey

mission

32 2013/11/15 毛淑德国家天文台研究员宇宙结构起源

33 2013/11/21 Youcai Zhang 中科院上海天文台博士

Alignments of galaxies

within cosmic filaments from

SDSS DR7

34 2013/12/16 吕建永南京信息工程大学教授

Global Simulation of the

solar wind-magnetosphere

interfaces: magnetopause

and open-closed boundary

35 2013/12/20 C.K. Shum

Geodetic Science at the

School of Earth Sciences,

and a Distinguished

University Scholar at The

Ohio State University

教授 Monitoring Mass Transports

from Space

36 2013/12/31 马寅哲 University of British

Columbia 博士

The density and velocity

field of galaxies


107

国际合作与台内学术报告统计

团组与学科片出访

人次占比

来访人

次占比

台内学

术报告占比

宇宙学、暗物质及高能天体物理研究 1 1% 0 0% 0 0%

宇宙伽玛暴、中子星及相关物理研究 0 0% 0 0% 0 0%

太阳高能及相关物理过程研究 7 5% 13 10% 4 11%

太阳活动的多波段观测研究 5 3% 6 5% 2 6%

暗物质和空间天文实验室 37 25% 34 27% 7 19%

暗物质和空间天文 50 34% 53 42% 13 36%

恒星结构、演化和脉动研究 0 0% 0 0% 0 0%

南极天文中心 11 7% 12 9% 0 0%

星系宇宙学和暗能量研究 6 4% 0 0% 6 17%

星系中的恒星形成研究 10 7% 11 9% 7 19%

分子云与恒星形成研究 22 15% 1 1% 2 6%

毫米波和亚毫米波技术实验室 20 14% 11 9% 3 8%

青海观测站 9 6% 0 0% 0 0%

南极天文和射电天文 78 53% 35 28% 18 50%

空间目标与碎片观测研究中心 7 5% 1 1% 1 3%

卫星精密定轨及应用研究 0 0% 0 0% 0 0%

CCD 相机研制实验室 0 0% 0 0% 0 0%

应用天体力学和空间目标与碎片 7 5% 1 1% 1 3%

近地天体探测和太阳系天体研究 3 2% 0 0% 2 6%

历算和天文参考系研究 4 3% 0 0% 0 0%

太阳和太阳系等离子体研究 0 0% 2 2% 2 6%

天体化学和行星科学实验室 0 0% 0 0% 0 0%

盱眙天文观测站 3 2% 1 1% 0 0%

行星科学和深空探测实验室（筹） 0 0% 2 2% 0 0%

行星科学和深空探测 10 7% 5 4% 4 11%

台领导 2 1% 33 26%

总计 147 100% 127 100% 36 100%


108

If you are interested in the work of PMO please contact division of Science & Technology Management at

+86-(0)25-83332288, 83332018 [email protected]


research annual report 2013 - cas · annual report’ î ì í3－content iii (50) constraints on...

Documents