Computer Science
Scientific paper
Mar 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008aipc..990..336p&link_type=abstract
FIRST STARS III: First Stars II Conference. AIP Conference Proceedings, Volume 990, pp. 336-338 (2008).
Computer Science
3
Population Ii Stars, Abundances, Chemical Composition, Stellar Structure, Interiors, Evolution, Nucleosynthesis, Ages, Supernovae
Scientific paper
We present a sample of s-process calculations at solar metallicity and at halo metallicity. First, for a 25 Msolar we report the weak s-process contribution to the elements between Co and Mo in the solar system. More than 50% of solar Cu, Ga, Ge and As is reproduced, and most of the solar elements between Fe and Sr receives a contribution higher than 10%. Second, we compare our results for the 25 Msolar obtained at low metallicity using three different initial distribution sets. We show that, just within the present uncertainties in the oxygen spectroscopic observations, s-process predictions change by about a factor of two at 1/10 of the solar metallicity and by a larger factor at 1/100 of the solar metallicity. Third, for 15, 20, 25 and 30 Msolar stars we report the isotopic distribution between Fe and Nb for different metallicities, where the same initial composition and nuclear network are used in the calculations. We show that the s-process efficiency changes star by star, and the s-process behavior with metallicity as well.
Gallino Roberto
Pignatari Marco
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