Morphology of synchrotron emission in young supernova remnants
Service d'Astrophysique, CEA Saclay, 91191 Gif-sur-Yvette, France
2 Department of Physics, North Carolina State University, Box 8202, Raleigh, NC 27695, USA e-mail: email@example.com
Accepted: 27 June 2005
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.
Key words: acceleration of particles / ISM: supernova remnants / ISM: cosmic rays / X-rays: ISM
© ESO, 2005