Statistics – Computation
Scientific paper
Oct 1987
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987apj...321..832m&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 321, Oct. 15, 1987, p. 832-845.
Statistics
Computation
71
Barium, Giant Stars, Heavy Elements, Metallic Stars, Neon Isotopes, Nuclear Fusion, Astronomical Models, Asymptotic Giant Branch Stars, Computational Astrophysics, Mass Transfer, Neutron Distribution, Neutron Sources, White Dwarf Stars
Scientific paper
Nuclear-reaction calculations of the heavy-element synthesis occurring in thermally pulsing asymptotic giant branch (AGB) stars were performed to analyze the observations of enhanced s-process elements in barium stars. In addition, s-process abundances were obtained from single neutron exposure calculations, and significant differences were found in the calculated abundances from previously published data. It was found that a mass transfer mechanism from an AGB star, in which the Ne-22 source operates, cannot be responsible for the s-process abundances observed in the classical barium stars HR 774 and Zeta Cap, and in the mild barium star Omicron Vir. A C-13 neutron source AGB star could better reproduce the abundance data of these stars. However, a potent C-13 neutron source has so far only been predicted to be active in low-metallicity AGB stars, and a low metallicity is not compatible with the population characteristics of the barium stars. Future observations needed to reconcile these findings are discussed.
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