WD+MS Systems as Progenitors of Type Ia Supernovae with Different Metallicities

Abstract

Abstract The single-degenerate model for the progenitors of type Ia supernovae (SNe Ia) is one of the two most popular models, in which a carbon–oxygen white dwarf accretes hydrogen-rich material from its companion, increases its mass to the Chandrasekhar mass limit, and then explodes as a SN Ia. Incorporating the prescription of Hachisu et al. (1999a, ApJ, 519, 314) for the accretion efficiency into Eggleton’s stellar evolution code and assuming that the prescription is valid for all metallicities, we carried out a detailed binary evolution study with different metallicities. We showed the initial and final parameter space for SNe Ia in a (log$ P$–$M_{\rm 2}$) plane. The positions of some famous recurrent novae in the (log$ P$–$M_{2}$) plane, as well as a supersoft X-ray source (SSS), RX J0513.9$-$6951 are well explained by our model, and our model can also explain the space velocity and mass of Tycho G, which is now suggested to be a companion star of Tycho’s supernova. Our study indicates that a SSS, V Sge, is a potential progenitor of supernovae, like SN 2002ic, if the delayed dynamical-instability model in Han and Podsiadlowski (2006, MNRAS, 368, 1095) is appropriate.