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

TL;DR

This study models the evolution of white dwarf binary systems across different metallicities to identify potential progenitors of Type Ia supernovae, explaining observed phenomena and specific candidate systems.

Contribution

It introduces a detailed binary evolution model incorporating accretion efficiency across all metallicities, expanding understanding of SNe Ia progenitors and explaining observed systems.

Findings

Model explains positions of recurrent novae and SSS RX J0513.9-6951 in parameter space.

Identifies Tycho G as a likely companion star of Tycho's supernova.

Suggests V Sge as a potential progenitor for certain supernovae.

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 (CO WD) 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) for the accretion efficiency into Eggleton's stellar evolution code and assuming that the prescription is valid for \emph{all} metallicities, we carried out a detailed binary evolution study with different metallicities. We show 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 ($\log P-M_{\rm 2}$) 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 the companion star of Tycho's supernova . Our study indicates that the SSS, V Sge, is a potential progenitor of supernovae like SN 2002ic if the delayed dynamical-instability model in Han & Podsiadlowski (2006) is appropriate.