The origin of non-thermal X-ray filaments and TeV emission in young SNRs

Abstract

At the early, ejecta dominated, stage of supernova remnant (SNR) expansion a fraction of the swept-up circumstellar magnetic field is dynamically compressed to approximate equipartition at the contact discontinuity separating the SN progenitor's wind (or the ISM) and the ejecta. We propose that the thin non-thermal X-ray filaments observed by the Chandra satellite in several young SNRs are associated with such ``pile-up'' of the magnetic field. We use a one-dimensional diffusion-convection transport equation to describe the propagation of non-thermal electrons near the contact discontinuity of a young SNR and to calculate spatially resolved emission spectra in the X-ray and TeV bands. The results suggest that the high-energy electrons are possibly accelerated at the forward shock, and emitting efficiently only when they diffuse into regions of high magnetic field near the contact discontinuity. Much more likely, though, is that they are locally accelerated at the contact discontinuity, in which case the acceleration cannot be related to Fermi-type processes and should occur due to other plasma mechanisms. As a consequence, the forward shock in young SNRs is inconspicuous and often unobservable, similar to that in the Crab nebular.

30 pages, 7 figs, submitted to ApJ

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• Magnetic draping of merging cores and radio bubbles in clusters of galaxies
• Characterizing the non-thermal emission of Cas A
• X-ray synchrotron emission from supernova remnants
• Diffuse, Non-Thermal X-ray Emission from the Galactic Star Cluster Westerlund 1
• Acceleration of cosmic rays by young core-collapse supernova remnants
• Non-Thermal X-ray Emission from the Northwestern Rim of the Galactic Supernova Remnant G266.2-1.2 (RX J0852.0-4622)
• Spectral softening in core-collapse supernova remnant expanding inside wind-blown bubble
• Radio polarimetry signatures of strong magnetic turbulence in Supernova Remnants
• Leptonic non-thermal emission from supernova remnants evolving in the circumstellar magnetic field
• Morphology of synchrotron emission in young supernova remnants
• Particle acceleration, escape and non-thermal emission from core-collapse supernovae inside non-identical wind-blown bubbles