Is the X-ray pulsating companion of HD 49798 a possible type Ia supernova progenitor?

TL;DR

This study investigates whether the white dwarf companion of HD 49798 is a potential progenitor of type Ia supernovae, using binary population synthesis to determine its composition and future evolution.

Contribution

The paper uses Monte Carlo binary population synthesis to assess the nature of HD 49798's companion, suggesting it is likely a CO white dwarf capable of producing an SN Ia.

Findings

HD 49798's companion is unlikely to be an ONe WD based on orbital period simulations.

The companion is most likely a CO WD that can reach Chandrasekhar mass by accreting He-rich material.

HD 49798 system may produce a type Ia supernova in the future.

Abstract

HD 49798 (a hydrogen depleted subdwarf O6 star) with its massive white dwarf (WD) companion has been suggested to be a progenitor candidate of type Ia supernovae (SNe Ia). However, it is still uncertain whether the companion of HD 49798 is a carbon-oxygen (CO) WD or an oxygen-neon (ONe) WD. A CO WD will explode as an SN Ia when its mass grows approach to Chandrasekhar mass, while the outcome of an accreting ONe WD is likely to be a neutron star. We followed a series of Monte Carlo binary population synthesis approach to simulate the formation of ONe WD + He star systems. We found that there is almost no orbital period as large as HD 49798 with its WD companion in these ONe WD + He star systems based on our simulations, which means that the companion of HD 49798 might not be an ONe WD. We suggest that the companion of HD 49798 is most likely a CO WD, which can be expected to increase its mass to the Chandrasekhar mass limit by accreting He-rich material from HD 49798. Thus, HD 49798 with its companion may produce an SN Ia in its future evolution.