Presentation #110.95 in the session “Stellar/Compact (Poster)”.
The exact nature of the progenitors of Type Ia supernovae remains obscure, despite the fact that the basic scenario of accretion-triggered white dwarf explosions in binary systems is well established. Some key properties of Type Ia supernova remnants, such as the radius and centroid energy of Fe Kα in the X-ray spectrum, are determined by the interaction between the ejecta and the ambient medium. We model the interaction between Chandrasekhar and sub-Chandrasekhar models for Type Ia supernova ejecta and circumstellar ejecta profiles sculpted by mass loss from SN Ia progenitors up to an age of 5000 years. We generate synthetic X-ray spectra from these supernova remnant models and compare their bulk properties at different expansion ages with X-ray observations from Chandra and Suzaku. We attempt to establish quantitative limits on the circumstellar environments in which Type Ia supernova occur to rule out potential progenitor scenarios.