Morphology of synchrotron emission in young supernova remnants

被引：8
|
作者：
Cassam-Chenaï, G
Decourchelle, A
Ballet, J
Ellison, DC
机构：
[1] CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France
[2] N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA
来源：
ASTRONOMY & ASTROPHYSICS | 2005年 / 443卷 / 03期
关键词：
acceleration of particles; ISM : supernova remnants; ISM : cosmic rays; X-rays : ISM;
D O I：
10.1051/0004-6361:20052853
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
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.
引用
收藏
页码：955 / U86
页数：8
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