Ｘ－Ｒａｙ　Ｏｂｓｅｒｖａｔｉｏｎｓ of SN1006 Koyama, Ｋ . 　　 Kyoto University

Palmieri et al (1972) Ballon : The first X-ray detectionWinkler and Laird : OSO7 The spectrum Photon index =2.3 　 or kT = 4 keVBecker 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

ＭｏｒｐｈｏｌｏｇｙＣｈａｎｄｒａ：　Ｖｅｒｙ　Ｔｈｉｎ　Ｆｉｌａｍｅｎｔｓ

ＳｐｅｃｔｒｏｓｃｏｐｙＳｕｚａｋｕＴｈｅｒｍａｌ　ｖｓ Ｎｏｎ－Ｔｈｅｒｍａｌ

Chandra: Thin Filaments (Bamba et al.)

In this region, electron returnsback (small: quick, large: slow)The thin filaments =diffusion to the shock normal is smallThe Efficiency of Particle 　 AccelerationNR: High ER: Low

A ping-pong ball gets speed (energy) by a rally 　 in a moving wallshock

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

updown

E0102-72

Suzaku: Launch:2005/7/10 　 XIS

Suzaku XIS-FISuzaku 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

Black : XIS-BIRed : average of 3 XIS-FIs

He-OH-O

Non-thermal emission

3 - 5 keV band

3-5 keVOVII band

See also PosterE1.4-0025-06

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.

Assuming CIE Plasma

kT = 　 constant He-O line is prportinal to the thin thermal flux.

North rim East rim

Inner region

Large Thermal FluxSteep Non Thermal

North rim

East rim

Inner

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

Hard to distinguish CIE vs NEITwo Local Minima at large ntand small nt

Gamma-mapkT-map

nt-map

NEI ResultsSupport

Smal

ler

Larg

er

Lo

wer

Larg

er

Hig

her

Smal

ler

ConclusionNorth Rim Low density High temp and Highly NEI better injector to the accelerator.

Flat Γ, Sharp 　 WuAcceleration efficiency　　 　 is high Total thermal energy of plasma becomes small

East Rim High density Low temp and Moderate NEI

Steep Γ, Slow WuAcceleration efficiency is low Total thermal energy of plasma remains large

Ｃｈａｎｄｒａ　Ｉｍａｇｅ

North Rim

East Rim

Japanese historical record of SN1006“Meigetsuki” (This page was written in 8th September, in 1230.)

「客星古現例」the ancient samples of “guest stars”.

Guest stars = comets, novae, or supernovae

SN1006

ToJiTemple

Teika

朱雀大路

　

Suzaku-Mon 　Gate

Palace

SaiJiTemple

Su

zaku A

v.

Rajyo-Mon 　Gate

Southern Sky from Kyoto in AD1006/05/01

Mars

Antares

SN1006

Sai-Ji To- Ｊｉ

ToJiTemple

Tomb of Teika

Ｋｏｙａｍａ

House of Teika

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/registration/registration.cgi

and go into proper action

End