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Morphology of synchrotron emission in young supernova remnants

Gamil Cassam-Chenai·Anne Decourchelle·Jean Ballet·Donald C. Ellison
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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.

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Gamil Cassam-Chenai, Anne Decourchelle, Jean Ballet, Donald C. Ellison. 2005-07-08. Morphology of synchrotron emission in young supernova remnants. https://doi.org/10.1051/0004-6361%3A20052853

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