Arthur Choplin
Are some CEMP-s stars the daughters of spinstars?
Choplin, Arthur; Hirschi, Raphael; Meynet, Georges; Ekström, Sylvia
Abstract
Carbon-enhanced metal-poor (CEMP)-s stars are long-lived low-mass stars with a very low iron content as well as overabundances of carbon and s-elements. Their peculiar chemical pattern is often explained by pollution from an asymptotic giant branch (AGB) star companion. Recent observations have shown that most CEMP-s stars are in binary systems, providing support to the AGB companion scenario. A few CEMP-s stars, however, appear to be single. We inspect four apparently single CEMP-s stars and discuss the possibility that they formed from the ejecta of a previous-generation massive star, referred to as the “source” star. In order to investigate this scenario, we computed low-metallicity massive-star models with and without rotation and including complete s-process nucleosynthesis. We find that non-rotating source stars cannot explain the observed abundance of any of the four CEMP-s stars. Three out of the four CEMP-s stars can be explained by a 25M? source star with vini ~ 500 km?s-1 (spinstar). The fourth CEMP-s star has a high Pb abundance that cannot be explained by any of the models we computed. Since spinstars and AGB predict different ranges of [O/Fe] and [ls/hs], these ratios could be an interesting way to further test these two scenarios. nuclear reactions, nucleosynthesis, abundances / stars: interiors / stars: chemically peculiar / stars: abundances / stars: massive
Journal Article Type | Article |
---|---|
Acceptance Date | Oct 16, 2017 |
Online Publication Date | Oct 16, 2017 |
Publication Date | 2017-11 |
Publicly Available Date | May 26, 2023 |
Journal | Astronomy and Astrophysics |
Print ISSN | 2329-1273 |
Publisher | Hans Publishers |
Peer Reviewed | Peer Reviewed |
Volume | 607 |
Article Number | L3 |
DOI | https://doi.org/10.1051/0004-6361/201731948 |
Keywords | nuclear reactions, nucleosynthesis, abundances, stars, interiors, chemically peculiar, massive |
Publisher URL | http://doi.org/10.1051/0004-6361/201731948 |
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