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Origin of CEMP stars: What helium and lithium can tell us about CEMP stars?

Meynet, Georges; Hirschi, Raphael; Ekstrom, Sylvia; Maeder, André; Georgy, Cyril; Eggenberger, Patrick; Chiappini, Cristina

Authors

Georges Meynet

Sylvia Ekstrom

André Maeder

Cyril Georgy

Patrick Eggenberger

Cristina Chiappini



Abstract

We show that the peculiar surface abundance patterns of Carbon Enhanced Metal Poor (CEMP) stars has been inherited from material having been processed by H- and He-burning phases in a previous generation of stars (hereafter called the ``Source Stars''). In this previous generation, some mixing must have occurred between the He- and the H-burning regions in order to explain the high observed abundances of nitrogen. In addition, it is necessary to postulate that a very small fraction of the carbon-oxygen core has been expelled (either by winds or by the supernova explosion). Therefore only the most outer layers should have been released by the Source Stars. Some of the CEMP stars may be He-rich if the matter from the Source Star is not too much diluted with the InterStellar Medium (ISM). Those stars formed from nearly pure ejecta would also be Li-poor.

Journal Article Type Conference Paper
Acceptance Date Jan 12, 2010
Online Publication Date Apr 23, 2010
Publication Date Jan 12, 2010
Journal Proceedings of the International Astronomical Union
Print ISSN 1743-9213
Electronic ISSN 1743-9221
Publisher Cambridge University Press
Peer Reviewed Peer Reviewed
Volume 268
Pages 141-146
DOI https://doi.org/10.1017/S1743921310003984
Keywords . stars: AGB, early-type, evolution – supernovae: general – Galaxy: halo – nucleosynthesis
Publisher URL https://www.cambridge.org/core/journals/proceedings-of-the-international-astronomical-union/article/what-helium-and-lithium-can-tell-us-about-cemp-stars/5AACDB885E00ECDE93196DA147268F61
Related Public URLs https://arxiv.org/abs/1001.1864

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