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Blue metal-poor stars

Published online by Cambridge University Press:  02 March 2005

George W. Preston  and
Christopher Sneden
George W. Preston
Affiliation:
Carnegie Observatories, 813 Santa Barbara Street, Pasadena, CA 91101, USA email: gwp@ociw.edu
Christopher Sneden
Affiliation:
Department of Astronomy and McDonald Observatory, University of Texas, Austin, TX 78712, USA email: chris@verdi.as.utexas.edu
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Abstract

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We review the discovery of blue metal-poor (BMP) stars and the resolution of this population into blue stragglers and intermediate-age Main-Sequence stars by use of binary fractions. We show that the specific frequencies of blue stragglers in the halo field and in globular clusters differ by an order of magnitude. We attribute this difference to the different modes of production of these two populations. We report carbon and $s$-process enrichment among very metal-poor field blue stragglers and discuss how this result can be used to further resolve field blue stragglers into groups formed during RGB and AGB evolution of their erstwhile primary companions.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Keywords

Binaries: spectroscopicblue stragglersstars: chemically peculiarstars: abundances
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2004 , Issue IAUS224 , July 2004 , pp. 403 - 410
Copyright
© 2004 International Astronomical Union