Inner-shell ionization, radiative losses and thermal conductivity in young SNRs

Self-consistent treatment of time-dependent ionization in hydrodynamical calculations of the X-ray emission from young supernova remnants has been performed. The novel feature of the calculations is that K_alpha lines from species produced by inner-shell collisional ionization are included. Parameters of the shocked ejecta are found from fitting the model spectrum to the observed one. The application of the method to Tycho SNR using the classical deflagration model W7 for the explosion enables us to well reproduce the observed X-ray spectra and radial brightness profiles of the remnant.Comment: 4 pages, 3 figure, accepted for publication in MNRA

Oxygen emission in remnants of thermonuclear supernovae as a probe for their progenitor system

Recent progress in numerical simulations of thermonuclear supernova explosions brings up a unique opportunity in studying the progenitors of Type Ia supernovae. Coupling state-of-the-art explosion models with detailed hydrodynamical simulations of the supernova remnant evolution and the most up-to-date atomic data for X-ray emission calculations makes it possible to create realistic synthetic X-ray spectra for the supernova remnant phase. Comparing such spectra with high quality observations of supernova remnants could allow to constrain the explosion mechanism and the progenitor of the supernova. The present study focuses in particular on the oxygen emission line properties in young supernova remnants, since different explosion scenarios predict a different amount and distribution of this element. Analysis of the soft X-ray spectra from supernova remnants in the Large Magellanic Cloud and confrontation with remnant models for different explosion scenarios suggests that SNR 0509-67.5 could originate from a delayed detonation explosion and SNR 0519-69.0 from an oxygen-rich merger.Comment: 8 pages, 4 figures, MNRAS accepte