A simple model for electron plasma heating in supernova remnants
D. Malyshev1, S. Gabici2,1, L. O'C. Drury1 and F. A. Aharonian1,3
Dublin Institute for Advanced Studies, 31 Fitzwilliam Place, Dublin 2, Ireland e-mail: email@example.com
2 Laboratoire APC, CNRS-UMR 7164, Université Paris 7, 10 rue A. Domon et Léonie Duquet, 75025 Paris Cedex 13, France
3 Max-Planck-Institut für Kernphysik, Saupfercheckweg 1, 69117 Heidelberg, Germany
Accepted: 28 June 2010
Context. Multiwavelength observations of supernova remnants can be explained within the framework of diffusive shock acceleration theory, which allows effective conversion of the explosion energy into cosmic rays. Although the models of nonlinear shocks describe reasonably well the nonthermal component of emission, certain issues, including the heating of the thermal electron plasma and the related X-ray emission, still remain open.
Aims. Study of electron heating in supernova remnants in the Sedov phase due to Coulomb exchange between protons and electrons.
Methods. Numerical solution of the equations of the Chevalier model for supernova remnant evolution, coupled with Coulomb scattering heating of the electrons.
Results. The electron temperature and the X-ray thermal Bremsstrahlung emission from supernova remnants have been calculated as functions of the relevant parameters. Since only the Coulomb mechanism was considered for electron heating, the values obtained for the electron temperatures should be treated as lower limits. Results from this work can be useful to constrain model parameters for observed SNRs.
Key words: shock waves / ISM: supernova remnants / radiation mechanisms: thermal
© ESO, 2010