The helium star donor channel for the progenitors of type Ia supernovae with different metallicities

TL;DR

This study systematically investigates how metallicity influences the helium star donor channel for type Ia supernovae, revealing that metallicity affects progenitor properties, birthrates, and delay times.

Contribution

It provides a comprehensive analysis of the helium star donor channel across various metallicities using stellar evolution and population synthesis models, highlighting metallicity's impact on SNe Ia progenitors.

Findings

Higher metallicity leads to larger initial donor star masses and orbital periods.

SN Ia birthrates increase with metallicity in star-forming galaxies.

SNe Ia occur earlier and have higher peak rates at higher metallicities in starburst scenarios.

Abstract

Context: The nature of type Ia supernovae (SNe Ia) is still unclear. Metallicities may have an important effect on their properties. Aims: In this paper, we study the He star donor channel towards SNe Ia comprehensively and systematically at various metallicities. Methods: Employing Eggleton's stellar evolution code with the optically thick wind assumption, we calculated about 10 000 WD + He star systems and obtained SN Ia production regions of the He star donor channel with metallicities Z=0.03, 0.02, 0.004 and 0.0001. According to a detailed binary population synthesis approach, we also obtained SN Ia birthrates at various metallicities. Results: Our study shows that both the initial mass of the He donor star and the initial orbital period for SNe Ia increase with metallicity, while the minimum initial mass of the carbon--oxygen white dwarfs producing SNe Ia decreases with metallicity. For a constant star-formation galaxy, SN Ia birthrates increase with metallicity. If a single starburst is assumed, SNe Ia occur systemically earlier and the peak value of the birthrate is larger for a high Z, and the He star donor channel with different metallicities can produce the young SNe Ia with delay times $\sim$45-220Myr.