Astronomy and Astrophysics – Astrophysics
Scientific paper
Jul 1998
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998acaps..18..276h&link_type=abstract
Acta Astrophys. Sin., Vol. 18, No. 3, p. 276 - 286
Astronomy and Astrophysics
Astrophysics
Barium Stars: Stellar Evolution, Barium Stars: Formation, Barium Stars: Galaxy, Barium Stars: Binaries
Scientific paper
Monte Carlo simulations of the model proposed in paper I are carried out and the results are compared with observations in this paper. The results show that most of the strong barium stars are generated from the channels of wind accretion, wind exposure and stable Roche-lobe overflow, while most of the mild ones are from wind accretion and wind exposure. As shown by the model, the orbital periods and pollution factors are correlated. The model also gives a Galactic birth-rate of barium stars of around 0.02 yr-1. The total number barium stars in the Galaxy brighter than the 10th apparent visual magnitude is estimated to be some 6000, the average mass of strong barium stars is estimated to be about 1.8 Msun, and the average mass of the white dwarf components is about 0.60 Msun. The results also support the views (a) that the thermal pulsation may begin at an earlier phase during the AGB than is usually assumed, (b) that a tidally enhanced stellar wind exists, and (c) that the maximum stellar mass for s-processing is about 2 Msun.
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