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Modelling the evolution and nucleosynthesis of carbon-enhanced metal-poor stars

Published online by Cambridge University Press:  01 April 2008

O. R. Pols ,
R. G. Izzard ,
M. Lugaro  and
S. E. de Mink
O. R. Pols
Affiliation:
Sterrekundig Instituut Utrecht, P. O. Box 80000, NL-3584 TA Utrecht, The Netherlands email: [email protected], [email protected], [email protected], [email protected]
R. G. Izzard
Affiliation:
Sterrekundig Instituut Utrecht, P. O. Box 80000, NL-3584 TA Utrecht, The Netherlands email: [email protected], [email protected], [email protected], [email protected]
M. Lugaro
Affiliation:
Sterrekundig Instituut Utrecht, P. O. Box 80000, NL-3584 TA Utrecht, The Netherlands email: [email protected], [email protected], [email protected], [email protected]
S. E. de Mink
Affiliation:
Sterrekundig Instituut Utrecht, P. O. Box 80000, NL-3584 TA Utrecht, The Netherlands email: [email protected], [email protected], [email protected], [email protected]
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Abstract

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We present the results of binary population simulations of carbon-enhanced metal-poor (CEMP) stars. We show that nitrogen and fluorine are useful tracers of the origin of CEMP stars, and conclude that the observed paucity of very nitrogen-rich stars puts strong constraints on possible modifications of the initial mass function at low metallicity. The large number fraction of CEMP stars may instead require much more efficient dredge-up from low-metallicity asymptotic giant branch stars.

Keywords

Stars: AGB and post-AGBstars: evolutionstars: binariesstars: abundancesstars: mass function
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Symposium S252: The Art of Modeling Stars in the 21st Century , April 2008 , pp. 383 - 389
Copyright
Copyright © International Astronomical Union 2008

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