the suzaku results of sn1006 koyama, K. 1, bamba, a. 2, yamaguchi, h. 1 1 kyoto university, 2...
Post on 29-Jan-2016
214 Views
Preview:
TRANSCRIPT
The Suzaku Results of SN1006 Koyama, K .1 , Bamba, A.2 , Yamaguchi, H.1
1Kyoto University, 2Rikken
Nickname Suzaku
AncientOriental mythology
ASTRO E2 Launch:
2005/7/10
3 Main Detectors : HXD, XRS, XIS
E0102-72
XIS
Suzaku XIS-FISuzaku XIS-BI
O VII
O VIII
Ne IX
Ne X
Good Response of low energy
Low and Stable BG at high energy
Galactic Center
Japanese historical record of SNR“Meigetsuki” (This page was written in 11/8, 1230.)
「客星古現例」the ancient samples of “guest stars”.
Guest stars = comets, novae, and supernovae
< ----------------------- chronological order 8 7 6 5 4 3 2 1
SN10063C58
Crab Nebula
3C58
Chandra image of 3C58
高倉院 治承五年 六月廿五日 庚午 戌時 客星見北方 近王良 守伝舎星
In the reign-period of Takakura-In, June 25th, 5th year of Jisyou (= August 7th, 1181), a guest star appeared in northern sky at 20:00. It was near to the star of “Oh-Ryo” (= real person’s name of ancient China) and “Densya”.
王良 (Oh-Ryo)Cassiopeiaβ
伝舎 (Densya) = Camelopardalis
Crab nebula
Chandra image of Crab
後冷泉院 天喜二年 四月中旬以降 丑時 客星觜参度 見東方 孛天関星 大如歳星
In the reign-period of Goreizei-In, after the middle of April, 2nd year of Tenki (= May-June, 1054), a guest star appeared
nearby “Shi” and “Shin” (= Orion) in eastern sky at 2:00. It shined near to the star of “Tenkan”, and its size was comparable to Jupiter.
觜 , 参 = Orion
天関 (Tenkan)Taurusζ
SN1006
Chandra image of SN1006
一條院 寛弘三年 四月二日 葵酉 夜以降 騎官中 有大客星 如螢惑 光明動耀 連夜正見南方 或云 騎陣将軍星本体 増変光
In the reign-period of Ichijo-In, April 2nd, 3rd year of Kanko (= May 1st, 1006), a great guest star appeared within the constellation “Kikan” (=Imperial Guards).It was very bright like Mars, and visible in the southern sky every night.
騎陣将軍 (Kijin-Shogun) Lupusκ
騎官 (kikan)
Narrow band images of XIS-BI
He-O line band 3 - 5 keV band
Distributions of thermal plasma (line emission) and non-thermal electron (synchrotron emission) are different !
Black : XIS-BIRed : average of 3 XIS-FIs
He-OH-O
Non-thermal emission
3 - 5 keV band
3-5 keV OVII band
See also PosterE1.4-0025-06
North rim
East rim
Inner
H-O
He-O
North rim
East rimInner region
H-O/He-O ~ 0.2 in all regions !
Line intensity: East rim > North rim → Density: East rim > North rimH-O/He-O ratio: East rim < North rim→ Temperature: East rim < North rim
CIE Plasma
He-O line vs. hard X-ray emission
North rim
East rim
Inner region Consistent with imaging analysis !
Chandra Image
North Rim
East Rim
Red : North Black : East
North Rim
East Rim
SN 1006: Non-Thermal Filaments (Bamba et al.)
(Preliminary) ResultsNorth Rim Low density High temp and Highly NEI Flat Γ Sharp Wu
East Rim High density Low temp and Moderate NEI Steep Γ Slow Wu
Acceleration efficiency vs Plasma Temp.
朱雀Suzaku
The wall painting of “Suzaku” i n the ancient tomb “Kitora”built in the Asuka Era
Southern Sky from Kyoto in AD1006/5/1
top related