(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

XMM-Newton 　 G32.45+0.1

α = 　 1.7 　NH = 3 ×1022

Red0.5-2 keV

Blue2-7 keV

Contour20 cm

Grey2-7 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

SN1006

Non-Thermal Shells

RCW 86

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

Magnetic field

Shock Front

Electron Trajectory

Up Stream

Down Stream

９０ °

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-Rays ＶｓRadio 　Contours （６ｃｍ）

14

Jet Velocity > 1000 km/s t age(1) < 5000 years

　　　　　　　　　　 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

The ENDThe END

ASCA Galactic Plane Survey

G11.0-0.1 G23.5-0.0 G25.5-0.0

G26.6-0.1 G28.6-0.1

Kepler

Cas A

Tycho　SNR

Non-Thermal Shellsfrom Thermal SNRs

uu　=　4ud　=2890　km/s m.f.p.　of　e　=　rg　

tloss:　energy　loss　time　scale　(synch.　loss)

　tacc:　acceleration　time　scale

~ 　　　　　　　 >　1dBB

-2

shockB

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