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Type Ia supernovae (SNe Ia) play a crucial role in studying cosmology andgalactic chemical evolution. They are thought to be thermonuclear explosions ofcarbon-oxygen white dwarfs (CO WDs) when their masses reach the Chandrasekarmass limit in binaries. Previous studies have suggested that He novae may beprogenitor candidates of SNe Ia. However, the mass retention efficienciesduring He nova outbursts are still uncertain. In this article, we aim to studythe mass retention efficiencies of He nova outbursts and to investigate whetherSNe Ia can be produced through He nova outbursts. Using the stellar evolutioncode Modules for Experiments in Stellar Astrophysics, we simulated a series ofmulticycle He-layer flashes, in which the initial WD masses range from 0.7 to1.35 Msun with various accretion rates. We obtained the mass retentionefficiencies of He nova outbursts for various initial WD masses, which can beused in the binary population synthesis studies. In our simulations, He novaoutbursts can increase the mass of the WD to the Chandrasekar mass limit andthe explosive carbon burning can be triggered in the center of the WD; thissuggests that He nova outbursts can produce SNe Ia. Meanwhile, the massretention efficiencies in the present work are lower than those of previousstudies, which leads to a lower birthrates of SNe Ia through the WD + He starchannel. Furthermore, we obtained the elemental abundances distribution at themoment of explosive carbon burning, which can be used as the initial inputparameters in studying explosion models of SNe Ia.

Mass retention efficiencies of He accretion onto carbon-oxygen white dwarfs and type Ia supernovae