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Paper: The Origin and Evolution of Helium-rich Hot Subdwarfs
Volume: 452, Fifth Meeting on Hot Subdwarf Stars and Related Objects
Page: 13
Authors: Zhang, X.; Jeffery, C. S.
Abstract: White dwarfs are thought to be the final evolutionary stage of most stars. They are frequently observed in binary systems, and a few of them have a white dwarf companion. Due to gravitational radiation, a double white dwarf binary will decay and may merge. In this paper, we describe the evolution following the merger of two helium white dwarfs. Our results demonstrate that a model comprising both fast accretion to form a (hot) corona, and slow accretion from a (cold) debris disk can reproduce the observed distribution of helium-rich subdwarfs in terms of their surface temperatures, gravities, nitrogen and carbon abundances.
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