Astronomy and Astrophysics – Astrophysics
Scientific paper
May 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992a%26a...258..357b&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 258, no. 2, p. 357-367.
Astronomy and Astrophysics
Astrophysics
28
Chemical Composition, Chemical Evolution, Galactic Evolution, Massive Stars, Nuclear Fusion, Stellar Mass, Heavy Elements, Metallicity, Milky Way Galaxy
Scientific paper
We investigate the s-process nucleosynthesis during the core helium burning phase of massive stars for various values of the initial metallicity (Z). Models of stars of masses 15, 20, and 30 solar masses with Z in the range of 10 exp -8 to 0.02 are calculated from the ZAMS to the end of core helium burning. An updated nuclear reaction network coupled to the stellar evolution code is used to follow the s-process nucleosynthesis. As in previous investigations, it is found that the production of most heavy elements does not depend linearly on metallicity; the relationship of Cu and Zn to the metallicity is, however, close to a linear one. As a new result, we find that the (C-13)(alpha, n)(O-16) neutron source becomes effective prior to the onset of core helium ignition in extremely metal-poor stars and leads to a significant production of some 'light' s-nuclei. Finally, we study the sensitivity of our results to the nuclear data and stellar conditions, and give yields of elements from Ni to Zr as a function of stellar mass and metallicity, to be used in models of the chemical evolution of the Galaxy.
Baraffe Isabelle
El Eid Mounib F.
Prantzos Nikos
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