A comprehensive progenitor model for SNe Ia

TL;DR

This paper models the evolution of white dwarf binaries to predict the initial conditions and birth rates of Type Ia supernovae, incorporating effects like mass-stripping and disk instability, and compares results with observations.

Contribution

It provides a comprehensive progenitor model for SNe Ia, including detailed initial parameter spaces and birth rate estimates based on binary evolution and population synthesis.

Findings

Initial parameter spaces for SNe Ia identified in orbital period-secondary mass plane.

Galactic SNe Ia birth rate estimated at 2.55-2.9×10^{-3} yr^{-1}, slightly below observations.

Delay time distribution shows weak bimodality with contributions from different channels.

Abstract

Incorporating the effect of mass-stripping and accretion-disk instability on the evolution of WD binary, we carried out binary stellar evolution calculations for more than 1600 close WD binaries. As a result, the initial parameter spaces for SNe Ia are presented in an orbital period-secondary mass ($\log P_{\rm i}, M_{\rm 2}^{\rm i}$) plane. We confirmed that in a WD + MS system, the initial companion leading to SNe Ia may have mass from 1 $M_{\odot}$ to 5 $M_{\odot}$. The initial WD mass for SNe Ia from WD + MS channel is as low as 0.565 $M_{\odot}$, while the lowest WD mass from the WD + RG channel is 1.0 $M_{\odot}$. Adopting the results above, we studied the birth rate of SNe Ia via a binary population synthesis approach. We found that the Galactic SNe Ia birth rate from SD model is $2.55 - 2.9\times10^{\rm -3}$ ${\rm yr}^{\rm -1}$ (including WD + He star channel), which is slightly smaller than that from observation. If a single starburst is assumed, the distribution of the delay time of SNe Ia from the SD model is a weak bimodality, where WD + He channel contribute to SNe Ia with delay time shorter than $10^{\rm 8}$ yr and WD + RG channel to those with age longer than 6 Gyr.