Computer Science – Numerical Analysis
Scientific paper
Mar 1980
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980apj...236..648c&link_type=abstract
Astrophysical Journal, Part 1, vol. 236, Mar. 1, 1980, p. 648-657. NSF-supported research.
Computer Science
Numerical Analysis
48
Barium, Metallic Stars, Nuclear Fusion, Numerical Analysis, Stellar Evolution, Abundance, Barium Isotopes, Dysprosium, Gadolinium, Independent Variables, Mathematical Models, Rare Earth Elements, Samarium
Scientific paper
Theoretical s-process calculations are presented. Isotopic abundances are summed, so that atomic number becomes the independent variable. This form of representation of the calculations has distinct advantages in the interpretation of stellar data, since one generally does not have isotopic information. Predictions based on single neutron exposures as well as exponential exposure distributions are compared with the high-quality observations of Tech (1971) for Zeta Cap and a few other stars. Tech's data provide a remarkably good fit of theory and observations. For the exposures of relevance to the barium stars, dysprosium and, indeed, heavier lanthanides are expected to be comparable in abundance to samarium and gadolinium. A very low Ce/Ba ratio (less than approximately 0.1) is not expected if Ba and Sr have comparable abundances. It is concluded that the observations are not yet of high enough quality to allow one to discriminate among several possible exposure models, but that the prospect for doing so with improved observations is good.
Cowley Ch. R.
Downs P. L.
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