%0 Journal Article %T Are some CEMP-s stars the daughters of spinstars? %A Arthur Choplin %A Georges Meynet %A Raphael Hirschi %A Sylvia Ekstr£¿m %J - %D 2017 %R 10.1051/0004-6361/201731948 %X 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¡Ñ 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 %U https://www.aanda.org/articles/aa/full_html/2017/11/aa31948-17/aa31948-17.html