1. Ｘ－Ｒａｙ Ｏｂｓｅｒｖａｔｉｏｎｓ of SN1006 Koyama, Ｋ. Kyoto University Palmieri et al (1972) Ballon : The first X-ray detection Winkler and Laird : OSO7 The spectrum Photon index =2.3 or kT = 4 keV Becker et al (1980) SSS, OSO8 : Crab Like spectrum : Photon index ＝ 2.2 (no line) Vartanian et al.1985 (GSPC: Balloon) Detection of OVII line = Thermal Plasma (0,1-0.2 keV) Koyama et al. 1987 (GSPC: Tenma) : Steeper Power law Photon index- 3.3 NEI Plasma kT 1.9 keV Ｍｏｒｐｈｏｌｏｇｙ Ｃｈａｎｄｒａ： Ｖｅｒｙ Ｔｈｉｎ Ｆｉｌａｍｅｎｔｓ Ｓｐｅｃｔｒｏｓｃｏｐｙ Ｓｕｚａｋｕ Ｔｈｅｒｍａｌ ｖｓ Ｎｏｎ－Ｔｈｅｒｍａｌ

2. Chandra: Thin Filaments (Bamba et al.) In this region, electron returns back (small: quick, large: slow) The thin filaments = diffusion to the shock normal is small The Efficiency of Particle Acceleration NR: High ER: Low A ping-pong ball gets speed (energy) by a rally in a moving wall shock

3. B (perpendicular) down stream becomes very turbulent, hence be strongly scattered. B=100 – 400  G (Berezhko et al. 2004) B (pararell) Strong B makes the gyro radius small → diffusion becomes small Efficient particle accelerations  Thermal plasma shock E= 50-80 TeV. B=10 – 20  G up down

4. E0102-72 Suzaku: Launch:2005/7/10 XIS Suzaku XIS-FI Suzaku XIS-BI O VII O VIII Ne IX Ne X BI: Good Response at low energy FI: Low and Stable BG at high energy Galactic Center

5. Black : XIS-BI Red : average of 3 XIS-FIs He-O H-O Non-thermal emission 3 - 5 keV band 3-5 keVOVII band See also Poster E1.4-0025-06

6. North rim East rim Inner We divide the NE rim region into 64 segments. Made each spectra Fit with a Power-law + thin plasma model Then.

7. Assuming CIE Plasma kT = constant He-O line is prportinal to the thin thermal flux. North rim East rim Inner region Large Thermal Flux Steep Non Thermal North rim East rim Inner

8. Results of the CIE Case (1) Stronger OVII Flux (Thermal flux) Region has a steeper gamma (Non Thermal) (2) 3 regions (NR, ER, Inner) are separated by the Hard X-ray Flux vs OVII flux map Ｃｈａｎｄｒａ Ｉｍａｇｅ North Rim East Rim This is CIE case However the plasma in a young SNR Is likely NIE. We then try NIE plasma

9. Hard to distinguish CIE vs NEI Two Local Minima at large nt and small nt

10. Gamma-map kT-map nt-map NEI Results Support Smaller Larger Lower Larger Higher Smaller

11. Conclusion North Rim Low density High temp and Highly NEI better injector to the accelerator. Flat Γ, Sharp W u  Acceleration efficiency is high  Total thermal energy of plasma becomes small East Rim High density Low temp and Moderate NEI Steep Γ, Slow W u  Acceleration efficiency is low  Total thermal energy of plasma remains large Ｃｈａｎｄｒａ Ｉｍａｇｅ North Rim East Rim

12. Japanese historical record of SN1006 “Meigetsuki” (This page was written in 8 th September, in 1230.) 「客星古現例」 the ancient samples of “guest stars”. Guest stars = comets, novae, or supernovae SN1006

13. ToJi Temple Teika Suzaku-Mon Gate Palace SaiJi Temple Suzaku Av. Rajyo-Mon Gate

14. Southern Sky from Kyoto in AD1006/05/01 Mars Antares SN1006 Sai-Ji To- Ｊｉ

15. ToJi Temple Tomb of Teika Ｋｏｙａｍａ House of Teika

16. 朱雀 Suzaku The wall painting of “Suzaku” ｉ n the ancient tomb “Kitora” built in the Asuka Era Since the dead line of paper submission is approaching, please visit here http://www-cr.scphys.kyoto-u.ac.jp/ conference/suzaku2006/conference/suzaku2006/registration/registration.cgi and go into proper action

17. End