Computer Science
Scientific paper
Dec 1987
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987msngr..50...37m&link_type=abstract
ESO Messenger (ISSN 0722-6691), Dec. 1987, v. 50, p. 37-40. SERC-supported research.
Computer Science
Abundance, Barium, Neutron Sources, Nuclear Fusion, Stellar Evolution, Asymptotic Giant Branch Stars, Density (Number/Volume), Magnesium, Mass Transfer
Scientific paper
The origin of the large s-process enhancements observed in Ba II stars remains one of the most fundamental challenges in stellar nucleosynthesis theory. Knowledge of the two crucial aspects of the s-process site, namely the neutron source and the neutron density, would allow strong constaints to be placed on any evolutionary hypothesis purporting to explain the Ba II star phenomenon. In this paper, spectroscopic observations of a large number of both northern and southern hemisphere Ba II stars are used to determine the neutron source and neutron density in the cool (K4) Ba II star HD 178717. The results are compared with the abundances predicted if mass transfer from an evolved AGB star has occurred. A neutron density of about 2 x 10 to the 7th/cu cm at the s-process site is found for HD 178717. If an AGB mass transfer mechanism is responsible for the s-process enhancements of Ba II stars, then this low neutron density implies that significant revisions of present low-mass AGB models are required.
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