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Study of the Helium Enrichment in Globular Clusters

Published online by Cambridge University Press:  13 April 2010

Aldo A. R. Valcarce  and
Márcio Catelan
Aldo A. R. Valcarce
Affiliation:
Pontificia Universidad Católica de Chile, Departamento de Astronomía y Astrofísica, Av. Vicuña Mackenna 4860, 782-0436 Macul, Santiago, Chile email: avalcarc@astro.puc.cl; mcatelan@astro.puc.cl
Márcio Catelan
Affiliation:
Pontificia Universidad Católica de Chile, Departamento de Astronomía y Astrofísica, Av. Vicuña Mackenna 4860, 782-0436 Macul, Santiago, Chile email: avalcarc@astro.puc.cl; mcatelan@astro.puc.cl
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Abstract

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Globular clusters (GCs) are spheroidal concentrations typically containing of the order of 105 to 106, predominantly old, stars. Historically, they have been considered as the closest counterparts of the idealized concept of “simple stellar populations.” However, some recent observations suggest than, at least in some GCs, some stars are present that have been formed with material processed by a previous generation of stars. In this sense, it has also been suggested that such material might be enriched in helium, and that blue horizontal branch stars in some GCs should accordingly be the natural progeny of such helium-enhanced stars. In this contribution we show that, at least in the case of M3 (NGC 5272), the suggested level of helium enrichment is not supported by the available, high-precision observations.

Keywords

Hertzsprung-Russell diagramstars: abundancesstars: evolutionstars: horizontal-branchglobular clusters: generalglobular clusters: individual (M3 = NGC 5272)
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S262: Stellar Populations – Planning for the Next Decade , August 2009 , pp. 27 - 30
Copyright
Copyright © International Astronomical Union 2010

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