Fine Structure of the Thermal and Non-Thermal X-Rays in the SN 1006 Shell

Abstract

The North Eastern shell of SN 1006 is the most probable acceleration site of high energy electrons (up to about 100 TeV) with the Fermi acceleration mechanism at the shock front. We resolved non-thermal filaments from thermal emission in the shell with the excellent spatial resolution of Chandra. The non-thermal filaments seem thin sheets with the scales of about 1 arcsec (0.01 pc) and about 20 arcsec (0.19 pc) upstream and downstream of the shock, respectively. In a simple diffusive shock acceleration (DSA) model with the magnetic field parallel to the shock normal, the downstream region should have a highly disordered magnetic field of 30-40 micro G. The width at the upstream side is extremely small, comparable to the gyro-radius of the maximum energy electrons. This result might imply that the possible scenario is not the conventional diffusive shock acceleration with a parallel magnetic field but that with a nearly perpendicular field or electron shock surfing acceleration.

arXiv comment6 pages, 10 figures, to be published in AdvSpaceRes (Proc. 34th COSPAR Assembly, Symposium E1.4), the paper with full resolution images in http://www-cr.scphys.kyoto-u.ac.jp/member/bamba/Proceeding/COSPAR2003.pdf

References in corpus (5)

• Supernova Remnants in the Sedov Expansion Phase: Thermal X-Ray Emission
• Discovery of TeV Gamma Rays from SN1006: Further Evidence for the SNR Origin of Cosmic Rays
• The SN 1006 Remnant: Optical Proper Motions, Deep Imaging, Distance, and Brightness at Maximum
• Nonthermal Electrons at High Mach Number Shocks: Electron Shock Surfing Acceleration
• Constraints On the Diffusive Shock Acceleration From the Nonthermal X-ray Thin Shells In SN1006 NE Rim

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• The connection between supernova remnants and the Galactic magnetic field: An analysis of quasi-parallel and quasi-perpendicular cosmic ray acceleration for the axisymmetric sample
• Vortical field amplification and particle acceleration at rippled shocks