📝 SummarXiv

Abstract

Barium (Ba) stars belong to binary systems that underwent mass transfer events. As a consequence, their envelopes were enriched with material synthesized in the interiors of their evolved companions via \textit{slow} neutron-capture nucleosynthesis, the $s$-process. As post-interacting binaries, Ba stars figure as powerful tracers of the $s$-process. In this study, we conduct a classical local thermodynamic equilibrium analysis for a sample of 180 Ba giant stars to find complementary insights for the $s$-process, in form of elemental abundances of carbon, nitrogen, and oxygen, as well as the $^{12}\rm{C}/^{13}\rm{C}$ ratio. We found carbon abundances systematically larger than those observed in normal giants, with [C/Fe] ratios ranging within from $-0.30$ to $+0.60$~dex. As expected, the [C/Fe] ratios increase for lower metallicity regimes and are strongly correlated with the average $s$-process abundances. Nitrogen abundances have a flat behavior around $\rm{[N/Fe]}\sim+0.50$~dex and are moderately correlated with sodium abundances. Except for HD~107541, the entire sample shows $\rm{C/O}<1$. We found $^{12}\rm{C}/^{13}\rm{C}<20$ for $\sim80\%$ of the sampled stars and $^{12}\rm{C}/^{13}\rm{C}>60$ for three objects.