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Recent observations suggest that some type Ia supernovae (SNe Ia) originatefrom the merging of two carbon-oxygen white dwarfs (CO WDs). Meanwhile, recenthydrodynamical simulations have indicated that the accretion-induced collapsemay be avoided under certain conditions when double WDs merge violently.However, the properties of SNe Ia from this violent merger scenario are highlydependent on a particular mass-accretion stage, the so-called WD + He subgiantchannel, during which the primary WD is able to increase its mass by accretingHe-rich material from a He subgiant before the systems evolves into a double WDsystem. In this article, we aim to study this particular evolutionary stagesystematically and give the properties of violent WD mergers. By employing theEggleton stellar evolution code, we followed a large number of binarycalculations and obtained the regions in parameter space for producing violentmergers based on the WD + He subgiant channel. According to these simulations,we found that the primary WDs can increase their mass by ~0.10-0.45 Msun duringthe mass-accretion stage. We then conducted a series of binary populationsynthesis calculations and found that the Galactic SN Ia birthrate from thischannel is about 0.01-0.4*10-3 yr-1. This suggests that the violent WD mergersfrom this channel may only contribute to ~0.3%-10% of all SNe Ia in our Galaxy.The delay times of violent WD mergers from this channel are >1.7 Gyr,contributing to the SNe Ia in old populations. We also found that the WD + Hesubgiant channel is the dominent way for producing violent WD mergers that maybe able to eventually explode as SNe Ia.

The violent white dwarf merger scenario for the progenitors of type Ia supernovae