Morphology of synchrotron emission in young supernova remnants
arXiv:astro-ph/0507194 · doi:10.1051/0004-6361:20052853
Abstract
In the framework of test-particle and cosmic-ray modified hydrodynamics, we calculate synchrotron emission radial profiles in young ejecta-dominated supernova remnants (SNRs) evolving in an ambient medium which is uniform in density and magnetic field. We find that, even without any magnetic field amplification by Raleigh-Taylor instabilities, the radio synchrotron emission peaks at the contact discontinuity because the magnetic field is compressed and is larger there than at the forward shock. The X-ray synchrotron emission sharply drops behind the forward shock as the highest energy electrons suffer severe radiative losses.
arXiv comment8 pages, 6 figures, Accepted for publication in A&A
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Cited by in corpus (9)
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- Morphological evidence for azimuthal variations of the cosmic ray ion acceleration at the blast wave of SN 1006
- Proper Motions and Brightness Variations of Nonthermal X-ray Filaments in the Cassiopeia A Supernova Remnant
- Radio emission and nonlinear diffusive shock acceleration of cosmic rays in the supernova SN 1993J
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