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Binary Populations of Carbon-Enhanced Metal-Poor Stars

Published online by Cambridge University Press:  05 March 2013

Robert G. Izzard ,
Evert Glebbeek ,
Richard J. Stancliffe  and
Onno Pols
Robert G. Izzard*
Affiliation:
Institut d'Astronomie et d'Astrophysique, Université Libre de Bruxelles, Boulevard du Triomphe, B-1050 Brussels, Belgium Sterrenkundig Instituut, Universiteit Utrecht, P.O. Box 80 000, NL-3508 TA Utrecht, The Netherlands
Evert Glebbeek
Affiliation:
Sterrenkundig Instituut, Universiteit Utrecht, P.O. Box 80 000, NL-3508 TA Utrecht, The Netherlands Department of Physics and Astronomy, McMaster University, Hamilton, Ontario, L8S 4M1, Canada
Richard J. Stancliffe
Affiliation:
School of Mathematical Sciences, PO Box 28M, Monash University, Victoria 3800, Australia Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge, CB3 0HA, UK.
Onno Pols
Affiliation:
Sterrenkundig Instituut, Universiteit Utrecht, P.O. Box 80 000, NL-3508 TA Utrecht, The Netherlands
*
FCorresponding author. Email: robert.izzard@ulb.ac.be
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Abstract

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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: halonucleosynthesisstars: abundancesstars: AGBstars: binaries
Type
CEMP Stars
Information
Publications of the Astronomical Society of Australia , Volume 26 , Issue 3 , 2009 , pp. 311 - 313
Copyright
Copyright © Astronomical Society of Australia 2009

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