Post-merger evolution of double helium white dwarfs and distribution of helium-rich hot subdwarfs
arXiv:2104.06817 · doi:10.1093/mnras/stab1063
Abstract
The mergers of double helium white dwarfs are believed to form isolated helium-rich hot subdwarfs. Observation shows that the helium-rich hot subdwarfs can be divided into two subgroups based on whether the surface is carbon-rich or carbon-normal. But it is not clear whether this distribution directly comes from binary evolution. We adopt the binary population synthesis (BPS) to obtain the population of single helium-rich hot subdwarfs according to the channel of double helium white dwarfs merger. We find that the merger channel can represent the two subgroups in the plane related to different masses of progenitor helium white dwarfs. For = 0.02, the birth rates and local density of helium-rich hot subdwarf stars by the mergers of two helium white dwarfs is and 290.0 at 13.7 Gyr in our Galaxy, respectively. The proportion of carbon-rich and carbon-normal helium-rich hot subdwarfs are 32 and 68, respectively.
arXiv comment6 pages, 4 figures, accepted by MNRAS, comments welcome!
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