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.
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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
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