On Possible Oxygen/Neon White Dwarfs: H1504+65 and the White Dwarf Donors in Ultracompact X-ray Binaries

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dc.creatorWerner, K.
dc.creatorHammer, N. J.
dc.creatorNagel, T.
dc.creatorRauch, T.
dc.creatorDreizler, S.
dc.date2004-10-28
dc.date.accessioned2026-07-07T02:15:33Z
dc.date.available2026-07-07T02:15:33Z
dc.descriptionWe discuss the possibility to detect O/Ne white dwarfs by evidence for Ne overabundances. The hottest known WD, H1504+65, could be the only single WD for which we might be able to proof its O/Ne nature directly. Apart from this, strong Ne abundances are known or suspected only from binary systems, namely from a few novae, and from a handful of LMXBs. We try to verify the hypothesis that the latter might host strongly ablated O/Ne WD donors, by abundance analyses of the accretion disks in these systems. In any case, to conclude on O/Ne WDs just by strong Ne overabundances is problematic, because Ne enrichment also occurs by settling of this species into the core of C/O WDs.
dc.description6 pages, to appear in "White Dwarfs", eds. D. Koester, S. Moehler, ASP Conf. Series
dc.identifierhttps://arxiv.org/abs/astro-ph/0410690
dc.identifierhttp://arxiv.org/abs/astro-ph/0410690
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/8447
dc.subjectAstrophysics
dc.titleOn Possible Oxygen/Neon White Dwarfs: H1504+65 and the White Dwarf Donors in Ultracompact X-ray Binaries
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