Binary Populations of Carbon-Enhanced Metal-Poor Stars

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Contents Vol 26(3)

doi:10.1071/AS08066

Binary Populations of Carbon-Enhanced Metal-Poor Stars

Robert G. Izzard ^A ^B ^F, Evert Glebbeek ^B ^C, Richard J. Stancliffe ^D ^E, Onno Pols ^B

^A Institut d’Astronomie et d’Astrophysique, Université Libre de Bruxelles, Boulevard du Triomphe, B-1050 Brussels, Belgium
^B Sterrenkundig Instituut, Universiteit Utrecht, P.O. Box 80 000, NL-3508 TA Utrecht, The Netherlands
^C Department of Physics and Astronomy, McMaster University, Hamilton, Ontario, L8S 4M1, Canada
^D School of Mathematical Sciences, PO Box 28M, Monash University, Victoria 3800, Australia
^E Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge, CB3 0HA, UK.
^F Corresponding author. Email: robert.izzard@ulb.ac.be





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Publications of the Astronomical Society of Australia 26(3) 311–313 http://dx.doi.org/10.1071/AS08066
Submitted: 14 December 2008 Accepted: 25 March 2009 Published online: 10 September 2009

Abstract

We construct binary-star population nucleosynthesis models of carbon-enhanced metal-poor (CEMP) stars. We compare the CEMP to extremely metal-poor (EMP) ratio of our models to the observed ratio and find it is an order of magnitude too small. Through an increase in the efficiency of third dredge-up in low-mass, low-metallicity, thermally-pulsing Asymptotic Giant Branch (TP-AGB) stars our models better match the observations.

Keywords: Galaxy: halo — nucleosynthesis — stars: abundances — stars: AGB — stars: binaries