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The recent discovery that the Fe-K line luminosities and energy centroidsobserved in nearby SNRs are a strong discriminant of both progenitor type andcircumstellar environment has implications for our understanding of supernovaprogenitor evolution. Using models for the chemical composition ofcore-collapse supernova ejecta, we model the dynamics and thermal X-rayemission from shocked ejecta and circumstellar material, modeled as an $r^{-2}$wind, to ages of 3000 years. We compare the X-ray spectra expected from thesemodels to observations made with the Suzaku satellite. We also model thedynamics and X-ray emission from Type Ia progenitor models. We find a cleardistinction in Fe-K line energy centroid between core-collapse and Type Iamodels. The core-collapse supernova models predict higher Fe-K line centroidenergies than the Type Ia models, in agreement with observations. We argue thatthe higher line centroids are a consequence of the increased densities found inthe circumstellar environment created by the expansion of the slow-moving windfrom the massive progenitors.

Are Models for Core-Collapse Supernova Progenitors Consistent with the Properties of Supernova Remnants?