Constraints on CEMP-no progenitors from nuclear astrophysics

Abstract

The CEMP-no stars are long-lived small mass stars presenting a very low iron content and overabundances of carbon with no sign or only very weak signs for the presence of s- or r-elements. Although the origin of that abundance pattern is still a matter of debate, it was very likely inherited from a previous massive star, that we shall call here the source star. We rely on a recent classification of CEMP-no stars arguing that some of them are made of a material processed by hydrogen burning that was enriched in products of helium burning during the nuclear life of the source star. We examine the possibility of forming CEMP-no stars with this material. We study the nucleosynthesis of the CNO cycle and the Ne-Na Mg-Al chains in a hydrogen burning single zone while injecting the helium burning products ${}^{12}$C, ${}^{16}$O, ${}^{22}$Ne and ${}^{26}$Mg. We investigate the impact of changing the density and temperature, as well as the injection rate. The nuclear reaction rates involving the creation and destruction of ${}^{27}$Al are also examined. ${}^{14}$N, ${}^{23}$Na, ${}^{24}$Mg and ${}^{27}$Al are formed when injecting ${}^{12}$C, ${}^{16}$O, ${}^{22}$Ne and ${}^{26}$Mg in the hydrogen burning zone. The ${}^{12}$C/${}^{13}$C ratio is constant under various conditions in the hydrogen burning zone. The predicted [Al/Fe] ratio varies up to $\sim 2$ dex depending on the prescription used for the reaction rates involving ${}^{27}$Al. The experiments we carried out support the view that some CEMP-no stars are made of a material processed by hydrogen burning, coming from a massive star experiencing mild-to-strong rotational mixing. During its burning, this material was likely enriched in helium burning products. No material coming from the carbon-oxygen rich core of the source star should be added to form the daughter star, otherwise the ${}^{12}$C/${}^{13}$C ratio would be largely above the observed range of values.

13 pages, 7 figures, accepted for publication in A&A

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