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The nature of type Ia supernovae (SNe Ia) is still unclear. EmployingEggleton's stellar evolution code with the optically thick wind assumption, wesystematically studied the He star donor channel of SNe Ia, in which acarbon-oxygen white dwarf accretes material from a He main-sequence star or aHe subgiant to increase its mass to the Chandrasekhar mass. We mapped out theinitial parameters for producing SNe Ia in the orbital period--secondary massplane for various WD masses from this channel. According to a detailed binarypopulation synthesis approach, we find that this channel can produce SNe Iawith short delay times (~100Myr) implied by recent observations. We obtainedmany properties of the surviving companions of this channel after SN explosion,which can be verified by future observations. We also find that the survivingcompanions from the SN explosion scenario have a high spatial velocity(>400km/s), which could be an alternative origin for hypervelocity stars(HVSs), especially for HVSs such as US 708.

The helium star donor channel for the progenitors of type Ia supernovae and their surviving companion stars