The Origin and Evolution of Helium-rich Hot Subdwarfs

Details The Origin and Evolution of Helium-rich Hot Subdwarfs The Origin and Evolution of Helium-rich Hot Subdwarfs

Mar 2012

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012aspc..452...13z&link_type=abstract

Fifth Meeting on Hot Subdwarf Stars and Related Objects, ASP Conference Series Vol. 452, proceedings of a workshop held at Stell

Astronomy and Astrophysics

Astronomy

Scientific paper

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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