1 / 22

Non-Thermal X-ray Filaments from SNRs and the Galactic Center

This study investigates the non-thermal X-ray filaments observed in supernova remnants (SNRs) and the Galactic Center. Results from ASCA, Chandra, and XMM observations are presented, highlighting the search for non-thermal SNRs and the profile of their filaments. Follow-up observations with Chandra and XMM are discussed, as well as the distribution of high-energy cosmic rays in the galactic plane.

claytonscott
Download Presentation

Non-Thermal X-ray Filaments from SNRs and the Galactic Center

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

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

  2. 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

  3. Contour 20 cm Color 2-7 keV Chandra G28.6-0.1 kT =0.7 Log(nt) = 10.4 NH = 7.4x1022 α =2.1 NH = 3.8x1022

  4. Red 0.5-2 keV Blue 2-7 keV XMM-Newton G32.45+0.1 α =1.7 NH = 3 ×1022 Contour 20 cm Grey 2-7 keV

  5. B A C D Chandra３０Dor C (LMC) Red 0.5-2 keV Blue 2-7 keV B C Photon index(α) A = 2.9 B = 2.7 C = 2.3 D = 2.5 A D

  6. Non-Thermal Shells RCW 86 SN1006

  7. Hwang et al. (2002) “filaments with small E.W.” +0.3 -0.2 G=3.1 +0.002 -0.002 wu=0.015 pc The non-thermal Filament has thin Profile +0.012 -0.009 wd=0.079 pc Tycho 30“ = 0.3pc

  8. Kepler wu=0.024 pc +0.008 -0.007 wd=0.019 pc +0.007 -0.006 1 5 10 Energy (keV) +0.2 -0.2 +0.2 -0.2 G=2.3 G=2.2 1 5 10 Energy (keV) wu=0.038 pc +0.015 -0.011 The thin Filaments are non-thermal wd=0.069 pc +0.017 -0.012 30“ = 0.7pc

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

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

  11. Restriction of parameters! known parameters: uu,nrolloff, wu,wd unknown parameters: Emax, Bu, Bd,hu, hd, q A. Age limited case B. Loss limited case tacc = tage < tloss tloss = tacc < tage wu = min {Ku/uu, (Kutcool)1/2} wu = Ku/uu wd = Kd/ud wd = max {udtcool, (Kdtcool)1/2} Both cases, Bd = Bu(cos2q+r2sin2q)1/2 nlolloff ~ BE2 hd < hu

  12. Analysis of the SN1006 shell MagneticField (microG) Age Limited Diffusive shock accelera- tion modelwith nearly perpendicular magnetic field. Age-limited E ~ 30-200 TeV Loss-limited E~ 20-50 TeV Loss Limited Maximum Electron Energy (TeV)

  13. 3 2 1 Non-Thermal X-RayFilaments The 3-8 keV band image with Chandra Senda et al. Γ= 2.1 NH = 8 x1022 Hcm-2 Non-thermal filament near the GC Sgr A* See also Wang et al. and Sakano et al.

  14. 3 2 1 From the morphology and spectrum, we suspect that the spots 1,2 and 3 are the non-thermal X-ray jets ejected from the GC Γ=1.5 , NH = 1.2 x1023 Hcm-2

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

  16. X-Ray Reflection Nebula(Sgr B2)6.4 keV map Simulation Sgr A* Sgr A* was bright about 300 years ago X-rays 5

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

  18. 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

  19. The END Thank You

  20. ASCA Galactic Plane Survey G11.0-0.1 G23.5-0.0 G25.5-0.0 G26.6-0.1 G28.6-0.1

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

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

More Related