A New Formation Mechanism for the Hottest Horizontal-Branch Stars

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dc.creatorSweigart, Allen V.
dc.creatorBrown, Thomas M.
dc.creatorLanz, Thierry
dc.creatorLandsman, Wayne B.
dc.creatorHubeny, Ivan
dc.date2002-07-16
dc.date.accessioned2026-07-07T02:04:20Z
dc.date.available2026-07-07T02:04:20Z
dc.descriptionStars with very large mass loss on the red-giant branch can undergo the helium flash while descending the white-dwarf cooling curve. Under these conditions the flash convection zone will mix the hydrogen envelope with the hot helium- burning core. Such ``flash-mixed'' stars will arrive on the extreme horizontal branch (EHB) with helium- and carbon-rich envelopes and will lie at higher temperatures than the hottest canonical (i.e., unmixed) EHB stars. Flash mixing provides a new evolutionary channel for populating the hot end of the EHB and may explain the origin of the high gravity, helium-rich sdO and sdB stars.
dc.description2 pages, Latex, 1 figure. To appear in "New Horizons in Globular Cluster Astronomy", eds. G. Piotto, G. Meylan, G. Djorgovski, & M. Riello, ASP Conference Series
dc.identifierhttps://arxiv.org/abs/astro-ph/0207343
dc.identifierhttp://arxiv.org/abs/astro-ph/0207343
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/4713
dc.subjectAstrophysics
dc.titleA New Formation Mechanism for the Hottest Horizontal-Branch Stars
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