The hybrid CONe WD + He star scenario for the progenitors of type Ia supernovae

TL;DR

This study explores the hybrid CONe white dwarf plus helium star scenario as a progenitor for type Ia supernovae, estimating birthrates, delay times, and potential links to type Iax supernovae through binary population synthesis.

Contribution

It provides the first detailed binary population synthesis analysis of the hybrid CONe WD + He star scenario for SNe Ia progenitors, including birthrates and delay times.

Findings

SN Ia birthrates are 0.033-0.539 per 10^(-3) yr, accounting for 1-18% of all SNe Ia.

Delay times range from 28 to 178 million years, the shortest among progenitor models.

Properties of donor stars at explosion offer insights for identifying surviving companions.

Abstract

The hybrid CONe white dwarfs (WDs) have been suggested to be possible progenitors of type Ia supernovae (SNe Ia). In this article, we systematically studied the hybrid CONe WD + He star scenario for the progenitors of SNe Ia, in which a hybrid CONe WD increases its mass to the Chandrasekhar mass limit by accreting He-rich material from a non-degenerate He star. According to a series of detailed binary population synthesis simulations, we obtained the SN Ia birthrates and delay times for this scenario. The SN Ia birthrates for this scenario are ~0.033-0.539*10^(-3)yr^(-1), which roughly accounts for 1-18% of all SNe Ia. The estimated delay times are ~28Myr-178Myr, which are the youngest SNe Ia predicted by any progenitor model so far. We suggest that SNe Ia from this scenario may provide an alternative explanation of type Iax SNe. We also presented some properties of the donors at the point when the WDs reach the Chandrasekhar mass. These properties may be a good starting point for investigating the surviving companions of SNe Ia, and for constraining the progenitor scenario studied in this work.