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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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