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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 Iasupernovae (SNe Ia). However, it is still uncertain whether the companion of HD49798 is a carbon-oxygen (CO) WD or an oxygen-neon (ONe) WD. A CO WD willexplode as an SN Ia when its mass grows approach to Chandrasekhar mass, whilethe outcome of an accreting ONe WD is likely to be a neutron star. We followeda series of Monte Carlo binary population synthesis approach to simulate theformation of ONe WD + He star systems. We found that there is almost no orbitalperiod as large as HD 49798 with its WD companion in these ONe WD + He starsystems based on our simulations, which means that the companion of HD 49798might not be an ONe WD. We suggest that the companion of HD 49798 is mostlikely a CO WD, which can be expected to increase its mass to the Chandrasekharmass limit by accreting He-rich material from HD 49798. Thus, HD 49798 with itscompanion may produce an SN Ia in its future evolution.

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