| Issue |
A&A
Volume 443, Number 3, December I 2005
|
|
|---|---|---|
| Page(s) | 955 - 959 | |
| Section | Interstellar and circumstellar matter | |
| DOI | https://doi.org/10.1051/0004-6361:20052853 | |
| Published online | 15 November 2005 | |
Morphology of synchrotron emission in young supernova remnants
1
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: gcassam@ncsu.edu
Received:
9
February
2005
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
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