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The nature of the progenitors of type Ia supernovae (SNe Ia) remains amystery. Binary systems consisting of a white dwarf (WD) and a main-sequence(MS) donor are potential progenitors of SNe Ia, in which a thermonuclearexplosion of the WD may occur when its mass reaches the Chandrasekhar limitduring accretion of material from a companion star. In the present work, weaddress theoretical rates and delay times of a specific MS donor channel to SNeIa, in which a He star+MS binary produced from a common envelope eventsubsequently forms a WD+MS system without the He star undergoing mass transferby Roche lobe overflow. By combining the results of self-consistent binaryevolution calculations with population synthesis models, we find that thecontribution of SNe Ia in this channel is around 2.0e-4 per year. In addition,we find that delay times of SNe Ia in this channel cover a range of about1.0-2.6 Gyr, and almost all SNe Ia produced in this way (about 97%) have adelay time of > 1 Gyr. While the rate of SN Ia in this work is about 10% of theoverall SN Ia rate, the channel represents a possible contribution to the oldpopulation (1-3 Gyr) of observed SNe Ia.

A closer look at non-interacting He stars as a channel for producing the old population of Type Ia supernovae