The Chemical Evolution of Helium in Globular Clusters: Implications for the Self-Pollution Scenario

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dc.creatorKarakas, Amanda
dc.creatorFenner, Yeshe
dc.creatorSills, Alison
dc.creatorCampbell, Simon
dc.creatorLattanzio, John
dc.date2006-08-17
dc.date.accessioned2026-07-07T10:39:48Z
dc.date.available2026-07-07T10:39:48Z
dc.descriptionWe investigate the suggestion that there are stellar populations in some globular clusters with enhanced helium (Y from 0.28 to 0.40) compared to the primordial value. We assume that a previous generation of massive Asymptotic Giant Branch (AGB) stars have polluted the cluster. Two independent sets of AGB yields are used to follow the evolution of helium and CNO using a Salpeter initial mass function (IMF) and two top-heavy IMFs. In no case are we able to produce the postulated large Y ~ 0.35 without violating the observational constraint that the CNO content is nearly constant.
dc.descriptionaccepted for publication in ApJ
dc.identifierhttps://arxiv.org/abs/astro-ph/0608366
dc.identifierhttp://arxiv.org/abs/astro-ph/0608366
dc.identifierAstrophys.J.652:1240-1245,2006
dc.identifierdoi:10.1086/508504
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/181155
dc.subjectAstrophysics
dc.titleThe Chemical Evolution of Helium in Globular Clusters: Implications for the Self-Pollution Scenario
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