1. Who accelerate cosmic rays
Koyama et al.(1995)
Discovery of sync. X-rays
from the shell of SN 1006
Koyama et al. (1997)：Sync. X-rays
Aharonian et al. (2004)：
　　　　　　　　　　　　VHE gamma-rays
SNR RXJ is an accelerator!
スペクトルからは磁場強度のみ、構造までみたければ …
高空間分解能観測　：Chandra (0.5 arcsec)
偏光観測　：将来の観測機器に期待

2. 1.4. Spectral Fitting Non-thermal! spectrum Hard No line SRCUT model
(keV)
power-law
exponential cutoff
Sync. emission from electrons
nrolloff = 5x1017Hz B
10mG
Emax
100TeV 2
Reynolds & Keohane (1999)
a = (fixed) (Allen et al. 2001)
nrolloff = 2.6 (1.9 – 3.3) x 1017 Hz
Flux = 1.8 x10-12 ergs cm-2s-1

3. 1.5. Many young historical SNRs have thin filaments with sync. X-rays
Cas A(SN1680)
Kepler(SN1604)
Tycho(SN1572)
SN1006
RCW 86
(SN184)
(Bamba et al.
2005)

4. Chandra: Thin Filaments (Bamba et al.)
In this region,
electron returns
back (small: quick,
large: slow)
The Efficiency of
Particle　
Acceleration
NR: High ER: Low？
A ping-pong
ball gets
speed (energy)
by a rally　in a
moving wall
Efficiency particle acceleration
Thermal plasma
shock

5. The scale length vs. radius2 5 10 50
Radius of SNR (pc)
10-2
10-1 1
Scale length (pc)
downstream
upstream
R/10
30 Dor C
RCW 86
Cas A
SN 1006
Tycho
R/1000
Kepler
The scale length is ~ % of the radius.

6. perpendicular B or parallel B ?
Why are filaments so thin?
….. Small diffusion in direction to shock normal!
perpendicular B or parallel B ?
Diffusion only occurs along the B
perpendicular!
ordered or turbulent B ?
turbulent → strongly scattered
　 → hardly go downstream
→ staying long around shocks
turbulent B
high effic.
(equipartition)
First quantitative image !
shock
Emax of electron TeV
The angle: > 85 deg.
The strength: 10 – 80 mG up
down

7. ９０° Magnetic field Up Stream Shock Front Electron Trajectory
Down Stream

8. another scenario very strong parallel B
(Berezhko et al. 2004)
Strong B makes the gyro radius small
→ diffusion becomes small
B ~ 100 – 400 mG
shock up
down
Turbulent magnetic field (Bohm limit)
Very efficient acceleration (equipartition)
Anyway,
First estimation of magnetic field structure

9. 未知の超新星残骸探査 硬X線探査 今までのSNR探査: 電波中心 (265個: Green et al. 2006) SN1006
1GHzでの表面輝度
(10-22W m-2Hz-1sr-1)
SN1006
銀河面からの距離 |b| (degree)
電波サーベイは銀河面近くで弱い
SN1006型は電波で暗い
硬X線探査

10. ASCAによる無バイアス銀河面探査 探査領域: 硬X線無バイアス探査としては |l| < 45o, |b| < 0.4o
おそらく最大･最高感度探査
複数の未同定宇宙線加速SNR候補を発見 G G G
Bamba et al. (2003b)
このようなSNR … ~20個?

11. ASCA Galactic Plane Survey

12. 2. HESS sources New accelerator candidates? :XIS Mapping Sgr A*
HESS J
HESS J
HESS J
HESS J
HESS J
HESS J
HESS J
HESS J
Aharonian et al. 2005
New
accelerator
candidates?
:XIS Mapping

13. HESS +
New SNRs

14. (1) RXJ /ＳＮ1006　: Hard Tail　
Prepared by T.Takahashi, J.Hiraga, K. Nakazawa、 Y.Uchiyama
Hard band
ACIS-I 3-5 keV
True TeV emitter
 ASCA GIS
Synchrotron X-ray
Uchiyama et al.
Aharonian et al.
SN1006 Γ~ 2.7 : the standard acceleration theory.
RXJ G~2.3 : hard to explain

15. Target list Name ext. flux* counterpart? viewing 1303-632 10 none
(HESS J…) (‘)
none
none - Oct.3
PSR J ? - Oct.3 G
G Oct.19
W33?
PSR ? - Oct.24 G
AX J ●
*: ergs/cm2/s above 200 GeV

16. Assumption: RX J1713 and HESS sources have same spectra
Who are they?
XIS spectra and image
detection with HXD?
Assumption: RX J1713 and HESS sources have same spectra
Name F2-10 keV
x10-12
x10-12
x10-12
x10-12
detectable with XIS 50ks
ASCA survey: 2x10-12ergs cm-2s-1
with 50ks
or strong upper limit…
If they are not RX J1713s.
Then dark accelerator !?

17. Suzaku will catch the nature of TeV unID sources
2.5. Suzaku observation of HESS unID sources
HESS J
HESS J
pos. of HESS J1804
(cal source)
(cal source)
2 – 7 keV
2 – 7 keV
strong upper limit !
(Matumoto et al.2006 )
dim counterpart ?
(Bamba et al. 2006)
Suzaku will catch the nature of TeV unID sources

18. Their nature is still unknown, but wide band obs. will solve it !
2.6. One possible scenario for TeV unID sources:
Emission from SNRs in various phases
young SNRs
(Yamazaki et al. astro-ph/ )
large shock speed
both e and p are accelerated
strong synchrotron X-rays
old SNRs
small shock speed
electrons are deccelerated
no emission
TeV unIDs are old SNRs
colliding with MCs?
Their nature is still unknown,
but wide band obs. will solve it !
SNRs colliding with MCs
amount of targets
strong p0 decay

19. FTeV/FX ratio target FTeV/FX Crab (PWN) ~2.7e-3 RX J1713 (SNR) ~0.06
HESS J ~8
HESS J >55?
HESS unID sourcesは
本当にproton acceleratorかもしれない!