Orbital elements of the mild and strong barium stars formed through a wind accretion scenario

Details Orbital elements of the mild and strong barium stars formed through a wind accretion scenario Orbital elements of the mild and strong barium stars formed through a wind accretion scenario

Apr 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008ap%26ss.314..351c&link_type=abstract

Astrophysics and Space Science, Volume 314, Issue 4, pp.351-359

Astronomy and Astrophysics

Astrophysics

Stars, Late-Type Stars, Chemical Peculiar Stars, Agb And Post Agb Stars, Mass-Loss Stars, Wind Accretion

Scientific paper

Taking account of the metallicity dependence of the s-process nucleosynthesis in the AGB stars, we adopted the wind accretion model with the condition of total angular momentum conservation and used the Monte-Carlo method to study the variations and the distributions of the orbital elements of the mild and strong Ba stars. The calculated results show that the level of heavy-element overabundance in a Ba star depends on the orbital period. Since there is a strong dependence of s-process yields on the initial stellar metallicity of the AGB star and a strong increase of the s-process yields in AGB stars with decreasing metallicity, the calculated results strongly suggest that the initial metallicity of the Ba star systems is another important parameter for the level of heavy-element overabundance in a Ba star. The strong Ba stars generally have lower metallicities than mild Ba stars. The masses of AGB progenitor and Ba star are other two parameters which also have some impact on the heavy-element overabundance in the Ba star.

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