Non Thermal Xray Filaments from SNRs and the

Non Thermal X-ray Filaments from SNRs and the Galactic Center K. Koyama & A. Bamba Kyoto University The Results of ASCA, Chandra and XMM (1) Search for Non-Thermal SNRs (2) Profile of the Non-Thermal Filaments of SNRs (3) Non Thermal X-Ray Filaments and X –Ray Jets from Sgr A* =>High Energy Particle Acceleration In all the SNRs & GC

ASCA Plane Survey G 11. 0+0. 0 α＝ 1. 6 NH=0. 8 x 1022 G 25. 5+0. 0 α＝ 1. 8 NH=2. 4 x 1022 G 26. 6 -0. 1 α＝ 1. 3 NH=0. 4 x 1022 G 28. 6 -0. 1 α＝ 2. 1 NH=2. 7 x 1022 G 32. 5+0. 1 α＝ 3. 3 NH=8 x 1022 G 38. 6+0. 0 α＝ 1. 1 NH=2. 0 x 1022 => Follow-up Observations with Chandra & XMM

Chandra G 28. 6 -0. 1 k. T = 0. 7 Log(nt) = 10. 4 NH = 7. 4 x 1022 Contour 20 cm Color 2 -7 ke. V α = 2. 1 NH = 3. 8 x 1022

XMM-Newton G 32. 45+0. 1 Red 0. 5 -2 ke. V Blue 2 -7 ke. V α = 1. 7 NH = 3 × 1022 Contour 20 cm Grey 2 -7 ke. V

Chandra ３０ Dor C (LMC) Red 0. 5 -2 ke. V Blue 2 -7 ke. V Photon index(α) A = 2. 9 B = 2. 7 C = 2. 3 D = 2. 5 B C A D A C B D

Non-Thermal Shells SN 1006 RCW 86

Tycho Hwang et al. (2002) “filaments with small E. W. ” G=3. 1 +0. 3 -0. 2 30“ = 0. 3 pc wu=0. 015 wd=0. 079 +0. 002 -0. 002 +0. 012 -0. 009 pc pc The non-thermal Filament has thin Profile

Kepler G=2. 2 1 +0. 2 -0. 2 5 10 Energy (ke. V) G=2. 3 wu=0. 024 +0. 008 pc -0. 007 wd=0. 019 +0. 007 pc -0. 006 +0. 2 -0. 2 30“ = 0. 7 pc 1 5 10 Energy+0. 015 (ke. V)pc =0. 038 wu -0. 011 wd=0. 069 +0. 017 pc -0. 012 The thin Filaments are non-thermal

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

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

known parameters: uu, nrolloff, wu, wd A. Age limited case tacc = tage < tloss wu = Ku/uu wd = Kd/ud unknown parameters: Emax, Bu, Bd, hu, hd, q B. Loss limited case tloss = tacc < tage wu = min {Ku/uu, (Kutcool)1/2} wd = max {udtcool, (Kdtcool)1/2} Both cases, Bd = Bu(cos 2 q+ r 2 sin 2 q)1/2 nlolloff ~ BE 2 hd < hu Restriction of parameters!

Analysis of the SN 1006 shell Age Limited Age-limited E ~ 30 -200 Te. V Loss-limited E~ 20 -50 Te. V Magnetic Field (micro. G) Diffusive shock acceleration model with nearly perpendicular magnetic field. Loss Limited Maximum Electron Energy (Te. V)

Non-Thermal X-Ray Filaments The 3 -8 ke. V band image with Chandra Senda et al. 3 2 1 Sgr A* Γ= 2. 1 NH = 8 x 1022 Hcm-2 Non-thermal filament near the GC See also Wang et al. and Sakano et al.

From the morphology and spectrum, we suspect that the spots 1, 2 and 3 are the non-thermal X-ray jets 2 ejected from the GC 3 1 Γ=1. 5 , NH = 1. 2 x 1023 Hcm-2

X-Rays Ｖｓ Radio Contours （６ｃｍ） Jet Velocity > 1000 km/s t age(1) < 5000 years 14

X-Ray Reflection Nebula (Sgr B 2) 6. 4 ke. V map Simulation Sgr A* 5 Sgr A* was bright about 300 years ago X-rays

Young SNR near at the GC (Sgr A East) Supernova exploded some 1000 s years ago The dense shocked shell arrived at the GC ~300 years ago S Ar Ca Thin Thermal spectrum SNR GC Fe

Distribution of High Energy Cosmic Rays (> 1019 e. V) 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 END

ASCA Galactic Plane Survey G 11. 0 -0. 1 G 26. 6 -0. 1 G 23. 5 -0. 0 G 25. 5 -0. 0 G 28. 6 -0. 1

Tycho SNR Non-Thermal Shells from Thermal SNRs Kepler Cas A

tloss: energy loss time scale (synch. loss) tacc: acceleration time scale q B up uu = 4 ud =2890 km/s shock down m. f. p. of e = hrg h~ d. B B -2 >1