EAS Publications Series
Volume 7, 2003Final Stages of Stellar Evolution
|Page(s)||217 - 217|
|Published online||15 May 2003|
C. Motch and J.-M. Hameury (eds)
EAS Publications Series, 7 (2003) 217
DSM/DAPNIA/SAp, CEA Saclay, 91191 Gif-sur-Yvette Cedex, France
This text is aimed at presenting the basic ingredients necessary to understand shell-type supernova remnants, with particular emphasis on their X-ray emission. The other observational domains (radio and optical) are mentioned but not discussed in depth. I do not discuss at all the synchrotron nebulae, such as the Crab Nebula, which are also relics of a supernova explosion, but are driven by the remaining pulsar rather than the mechanical energy of the supernova. After a brief historical introduction, I describe the hydrodynamic concepts used for supernova remnants. Then I describe the Sedov model governing middle-aged supernova remnants, and the coronal conditions under which the X-ray emission is computed. Quantitative formulae are given for the Sedov model, allowing to relate X-ray observations to energy, ambient density and age. A chapter describes the initial (young) and final (old) stages of supernova remnants. Cosmic-ray acceleration at shocks is described, as well as its consequences on supernova remnants. The final chapter deals with statistical issues.
© EAS, EDP Sciences, 2003
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