On the Evolutionary Status of Extremely Hot Helium Stars - are O(He) Stars Successors of RCrB Stars?

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dc.creatorRauch, Thomas
dc.creatorReiff, Elke
dc.creatorWerner, Klaus
dc.creatorHerwig, Falk
dc.creatorKoesterke, Lars
dc.creatorKruk, Jeff W.
dc.date2004-10-28
dc.date.accessioned2026-07-07T02:15:33Z
dc.date.available2026-07-07T02:15:33Z
dc.description95% of all stars end their lives as white dwarfs. About 20% of the hot post-AGB stars are hydrogen deficient. Most of these are the result of a late helium-shell flash, but the evolutionary status of a fraction of about 10-20% of the hottest hydrogen-deficient stars, namely four O(He) stars, is as yet unexplained. They could be the long-searched hot successors of RCrB stars, which have not been identified up to now. If this turns out to be true, then a third post-AGB evolutionary sequence is revealed, which is probably the result of a double degenerate merging process. More generally, understanding details of merging double degenerate stars is of interest in the context of SN Ia events and hence cosmology.
dc.description3 pages, 1 figure, proceedings "Astrophysics in the Far Ultraviolet", Aug 2004, Victoria, Canada
dc.identifierhttps://arxiv.org/abs/astro-ph/0410698
dc.identifierhttp://arxiv.org/abs/astro-ph/0410698
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/8449
dc.subjectAstrophysics
dc.titleOn the Evolutionary Status of Extremely Hot Helium Stars - are O(He) Stars Successors of RCrB Stars?
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