Statistics – Computation
Scientific paper
Mar 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...387..263r&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 387, March 1, 1992, p. 263-275.
Statistics
Computation
46
Massive Stars, Metallic Stars, Metallicity, Nuclear Astrophysics, Computational Astrophysics, Nuclear Fusion, Stellar Cores, Stellar Models
Scientific paper
The s-process in massive stars is analyzed as a function of metallicity. The nucleosynthesis occurring in both core helium and shell carbon burning is investigated by numerically modeling nuclear reaction networks, subject to the conditions provided by stellar models. The s-process in massive stars is found to be 'secondary-like' in the disk, the amount of s-process matter ejected being roughly proportional to Fe. In the halo, the s-efficiency drops at low metallicities, with Fe/H below about -2. The elemental s-contributions from massive stars to the solar abundances from iron to zirconium are presented. It is concluded that the weak component can account for a consistent fraction of the solar Cu, Ga, Ge, and Se. The evolutionary trends of elements such as Co, Ni, Cu, Zn, Rb, Sr, Y, and Zr are discussed in comparison with observations of stars belonging to the halo, where massive stars give their major imprint.
Busso Maurizio
Gallino Roberto
Raiteri Claudia M.
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