(2)(2) ProfileProfile ofof the Non-Thermalthe Non-Thermal Filaments of SNRsFilaments of SNRs
=>High Energy Particle Acceleration =>High Energy Particle Acceleration In all the SNRsIn all the SNRs & GC & GC
Non Thermal X-ray Non Thermal X-ray Filaments Filaments from from SNRs and the Galactic CenterSNRs and the Galactic Center
K. Koyama & A. Bamba K. Koyama & A. Bamba Kyoto UniversityKyoto University
(1) (1) Search for Non-Thermal SNRsSearch for Non-Thermal SNRs
(3) (3) Non Thermal X-Ray FilamentsNon Thermal X-Ray Filaments and X –Ray JetsX –Ray Jets from Sgr A*from Sgr A*
The Results of ASCA, Chandra and XMMThe Results of ASCA, Chandra and XMM
ASCA Plane Survey
G11.0+0.0 α = 1.6 NH=0.8 x1022
G25.5+0.0 α = 1.8 NH=2.4 x1022 G26.6-0.1 α = 1.3 NH=0.4x1022
G28.6-0.1 α = 2.1 NH=2.7x1022
G32.5+0.1 α = 3.3 NH=8 x1022
G38.6+0.0 α = 1.1 NH=2.0x1022 => Follow-up Observations with Chandra & XMM
Chandra G28.6-0.1
α = 2.1 NH = 3.8x1022
kT = 0.7 Log(nt) = 10.4 NH = 7.4x1022
Contour20 cmColor2-7 keV
B
C
DA
Chandra 30 Dor C (LMC)
B
DC
A
Red0.5-2 keV
Blue2-7 keV
Photon index(α) A = 2.9 B = 2.7 C = 2.3 D = 2.5
Tycho
30“ = 0.3pc
wd=0.079 pc+0.012-0.009
wu=0.015 pc+0.002-0.002
Hwang et al. (2002)
“filaments with small E.W.”
=3.1+0.3-0.2
The non-thermalFilament has thin Profile
Kepler
30“ = 0.7pc
+0.007-0.006wd=0.019 pc
wu=0.024 pc+0.008-0.007
=2.2+0.2-0.2
Energy (keV)1 5 10
The thin Filamentsare non-thermal
wd=0.069 pc+0.017-0.012
wu=0.038 pc+0.015-0.011
Energy (keV)1 5 10
=2.3+0.2-0.2
The scale length vs. radius
The scale length is ~ % of the radius.
2 5 10 50Radius of SNR (pc)
10-2
10-1
1
Scale length (pc)
downstreamupstream
Cas A
30 Dor C
RCW 86
SN 1006
Kepler
Tycho
R/1000
R/10Down Stream
Up Stream
A. Age limited case B. Loss limited casetacc = tage < tloss tloss = tacc < tage
wu = Ku/uu
wd = Kd/ud
wu = min {Ku/uu, (Kutcool)1/2}wd = max {udtcool, (Kdtcool)1/2}
unknown parameters: Emax, Bu, Bd, u, d,
known parameters:uu, rolloff, wu,wd
Bd = Bu(cos2+ r2sin2)1/2
lolloff ~ BE2
d < u
Both cases,
Restriction of parameters!
Maximum Electron Energy (TeV)
Magnetic F
ield (microG
)
Age Limited
Loss Limited
Diffusive shock accelera-tion model with nearly perpendicular magnetic field.
Age-limited E ~ 30-200 TeVLoss-limited E~ 20-50 TeV
Analysis of the SN1006 shell
Non-Thermal X-Ray FilamentsThe 3-8 keV band image with Chandra Senda et al.
1
2
3
Γ= 2.1 NH = 8 x1022 Hcm-2
Sgr A*Non-thermal filament near the GC
See also Wang et al. and Sakano et al.
1
Γ=1.5 , NH = 1.2 x1023 Hcm-2
From the morphology and spectrum, we suspect thatthe spots 1,2 and 3 arethe non-thermal X-ray jets ejected from the GC
2
3
X-Ray Reflection NebulaX-Ray Reflection Nebula (Sgr B2)(Sgr B2) 6.4 keV map 6.4 keV map SimulationSimulation
X-rays
Sgr A*
5
Sgr A* was bright about 300 years ago
Young SNR near at the GC (Sgr A East)Young SNR near at the GC (Sgr A East)
Thin Thermalspectrum
S Ar Ca Fe
GCSNR
Supernova exploded some 1000 s years ago
The dense shocked shell arrived at the GC ~300 years ago
Distribution of High Energy Cosmic Rays (> 1019 eV) From ICRR Home Page
No Data
The non-thermal X-ray filaments &Jets would be the same origin of high energy cosmic rays at the GC