A re-analysis of the heavy-element abundance of barium stars.

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Barium Stars: Element Abundances, Barium Stars: Heavy Elements

Scientific paper

On the basis of conservation of total angular momentum in a binary system including escaping matter, the authors adopt a model in which the companion star accretes matter from the main star through successive pulses with mixing in its outer envelope. From a self-consistent calculation of the heavy element overabundance of barium stars, it is found that, for an actual accretion rate equal to 1/5 the Bondi-Hoyle accretion rate, the calculated curves agree with the observed overabundances in a majority of barium systems with long orbital periods (P > 1600 d), while for two stars, HD 20405 and HD 16458, agreement is obtained if the accretion rate is increased to 1/2 the Bondi-Hoyle value. This indicates that the actual accretion rate is between 0.1 - 0.5 the Bondi-Hoyle rate. For short period (P < 600 d) stars, the agreement is not good. Thus, wind accretion appears plausible for barium stars with longer periods, while for the shorter period barium stars some other mechanism may be at work.

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