Models for extremely metal-poor halo stars

Simple item page
dc.creatorWeiss, A.
dc.creatorSchlattl, H.
dc.creatorSalaris, M.
dc.creatorCassisi, S.
dc.creator;
dc.date2004-02-13
dc.date.accessioned2026-07-07T02:12:17Z
dc.date.available2026-07-07T02:12:17Z
dc.descriptionTwo alternative scenarios concerning the origin and evolution of extremely metal-poor halo stars are investigated. The first one assumes that the stars have been completely metal-free initially and produced observed carbon and nitrogen overabundances during the peculiar core helium flash typical for low-mass Population-III stars. The second scenario assumes that the initial composition resulted from a mixture of primordial material with ejecta from a single primordial supernovae. Both scenarios are shown to have problems in reproducing C, N, and O abundances simultaneously, and both disagree with observed 12C/13C-ratios,though in different directions. We concentrate on the most iron-poor, carbon-rich object of this class, HE0107-5240, and conclude that the second scenario presently offers the more promising approach to understand these objects, in particular because evolutionary tracks match observations very well.
dc.descriptionsubmitted to Astron. Astrophys., 9 pages, 3 figures
dc.identifierhttps://arxiv.org/abs/astro-ph/0402334
dc.identifierhttp://arxiv.org/abs/astro-ph/0402334
dc.identifierAstron.Astrophys. 422 (2004) 217-223
dc.identifierdoi:10.1051/0004-6361:20040248
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/7396
dc.subjectAstrophysics
dc.titleModels for extremely metal-poor halo stars
dc.typetext

Files

Collections

arXiv