EDP Sciences
Free access
Volume 443, Number 3, December I 2005
Page(s) 955 - 959
Section Interstellar and circumstellar matter
DOI http://dx.doi.org/10.1051/0004-6361:20052853

A&A 443, 955-959 (2005)
DOI: 10.1051/0004-6361:20052853

Morphology of synchrotron emission in young supernova remnants

G. Cassam-Chenaï1, 2, A. Decourchelle1, J. Ballet1 and D. C. Ellison2

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