Supernova Remnants in the Sedov Expansion Phase: Thermal X-Ray Emission

Details Supernova Remnants in the Sedov Expansion Phase: Thermal X-Ray Emission Supernova Remnants in the Sedov Expansion Phase: Thermal X-Ray Emission

2000-08-03

arxiv.org/abs/astro-ph/0008066v1

Astronomy and Astrophysics

Astrophysics

19 pages, 11 figures, submitted to Astrophysical Journal

Scientific paper

10.1086/319011

Improved calculations of X-ray spectra for supernova remnants (SNRs) in the Sedov-Taylor phase are reported, which for the first time include reliable atomic data for Fe L-shell lines. This new set of Sedov models also allows for a partial collisionless heating of electrons at the blast wave and for energy transfer from ions to electrons through Coulomb collisions. X-ray emission calculations are based on the updated Hamilton-Sarazin spectral model. The calculated X-ray spectra are succesfully interpreted in terms of three distribution functions: the electron temperature and ionization timescale distributions, and the ionization timescale averaged electron temperature distribution. The comparison of Sedov models with a frequently used single nonequilibrium ionization (NEI) timescale model reveals that this simple model is generally not an appropriate approximation to X-ray spectra of SNRs. We find instead that plane-parallel shocks provide a useful approximation to X-ray spectra of SNRs, particularly for young SNRs. Sedov X-ray models described here, together with simpler plane shock and single ionization timescale models, have been implemented as standard models in the widely used XSPEC v11 spectral software package.

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