太陽雑誌会速報 2004.05.24 t.t.ishii
DESCRIPTION
太陽雑誌会速報 2004.05.24 T.T.Ishii. The Astrophysical Journal, 607:L131–L134 , 2004 June 1 NEAR-INFRARED OBSERVATIONS AT 1.56 MICRONS OF THE 2003 OCTOBER 29 X10 WHITE-LIGHT FLARE Yan Xu , 1 Wenda Cao, 1,2 Chang Liu, 1 Guo Yang, 1 - PowerPoint PPT PresentationTRANSCRIPT
1
太陽雑誌会速報2004.05.24
T.T.IshiiThe Astrophysical Journal, 607:L131–L134, 2004 June 1
NEAR-INFRARED OBSERVATIONS AT 1.56 MICRONS OF THE 2003 OCTOBER 29 X10 WHITE-LIGHT FLARE
Yan Xu,1 Wenda Cao,1,2 Chang Liu,1 Guo Yang,1 Jiong Qiu,1,2 Ju Jing,1 Carsten Denker,1,2 and Haimin Wang1,2
Received 2004 March 12; accepted 2004 April 22; published 2004 May 4
1 Center for Solar-Terrestrial Research, New Jersey Institute of Technology,
2 Big Bear Solar Observatory
2
Near-infrared (NIR/1.6m) image of the X10 flare
Dunn Solar Telescope at Sac Peakwith high-order AO(adaptive optics)
FOV: 91”×91”CCD: 1024×1024→0.0089”/pixel
2003-Oct-2920:42 UTFlare onset: 20:37peak: 20:49
3
NIR time sequence of the X10 flare with RHESSI HXR contour from 20:40 to 20:47 (1 image / 1 min.)
Blue: RHESSI HXR contour (50-100 keV channel)Red: local NIR intensity maxima (flare ribbons in NIR)
4
Temporal evolution of the NIR flare ribbonson SOHO/MDI longitudinal magetogram
Separation speed: 38 km/s within weak field (700 G), 19 km/s (1400G)
5
Forbes & Priest (1984) and Forbes & Lin (2000)Ec : electric field strength along the current sheet vt : ribbon separation speedBn: longitudinal magnetic field (near disk center)
⇒ Ec= 45 V/cm (much larger than previous results)
Intensity enhancement (18-25 % to quiet-Sun in NIR)→ temperature perturbation Wang et al. (1998)
→ radiative loss
⇒ 1031 ergs within 8 minutes
6
The Astrophysical Journal, 607:L59–L62, 2004 May 20
ON THE ORIGIN OF SOLAR FACULAE
C. U. Keller,1,2 M. Schüssler,1 A. Vögler,1
and V. Zakharov1
Received 2004 March 9; accepted 2004 April 5; published 2004 April 22
1 Max-Planck-Institut für Aeronomie
2 On sabbatical leave from the National Solar Observatory
太陽雑誌会速報2004.05.24
T.T.Ishii
7http://www.linmpi.mpg.de/~msch/Thesis_Voegler.pdf
ab initio three-dimensional simulations of nongray radiative magnetoconvectionin the solar surface layers with the MURaM code
(Max-Planck Institute for Aeronomy and University of Chicago Radiative Magnetohydrodynamics code)
Numerical MHD simulations
(100×288×288 grid points)
8
ObservationLites et al. 2004LaPalma1m Swedish Solar Telescope
SimulationB=400G = 60 deg.(viewing angle)
Upward = Limb-ward
9
Bright wall modelContinuum intensity &Slices of physical quantities(dash line: continuum level)
→Limb-ward