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The abundances of the slow neutron-capture (s-) process elements observed inbarium stars can be explained by considering mass transfer in a binary systemfrom an asymptotic giant branch (AGB) star onto a smaller mass and less evolvedbinary companion star. Based on the abundances of neutron-capture elements thebarium stars are broadly divided into two categories, "strong" and "mild"barium stars. However, an understanding of the role of the characteristicproperties of the companion AGBs on the formation of the different types ofbarium stars is still lacking. This work focuses on investigating the role ofthe mass of the companion AGB stars in this context. In a recenthigh-resolution spectroscopic study, we studied in detail the chemicalcomposition of a few barium stars that we have identified. In order tounderstand the nature and the mass of the companion stars, we first estimatedthe mass of these objects and then used a parametric model-based analysis toderive the masses of the primary companion stars. The calculation is extendedto 205 barium stars taken from literature. An analysis of the mass distributionrevealed that both the strong and the mild barium stars occupy the same rangeof masses. However, their companion AGB stars' mass distributions peak at twodifferent values 2.5 M$_{\odot}$ and 3.7 M$_{\odot}$, for the strong and themild barium stars respectively. This provides clear evidence that the formationof mild and strong Ba stars is greatly influenced by the initial masses of thecompanion AGB stars. It remains, however, to be seen the possible impact ofother factors such as orbital period and metallicity on the formation scenariosof barium stars.

Formation scenarios of Ba stars: new evidence from the masses of the companion AGBs