Dynamics and Radiation of Young Type-Ia Supernova Remnants: Important Physical Processes

Abstract

We analyze the physical processes that should be taken into account when modeling young type-Ia supernova remnants (SNRs) with ages of several hundred years in which forward (into the interstellar medium) and reverse (into the ejection) shocks propagate. We show that the energy losses in a heavy-element-rich ejection can be significant for SNRs even at this evolutionary phase. We study the effects of electron thermal conduction and the rate of energy exchange between electrons and ions on the temperature distribution and the X-ray emission from such SNRs.