S-process nucleosynthesis in massive stars and the weak component. I - Evolution and neutron captures in a 25 solar mass star

Details S-process nucleosynthesis in massive stars and the weak component. I - Evolution and neutron captures in a 25 solar mass star S-process nucleosynthesis in massive stars and the weak component. I - Evolution and neutron captures in a 25 solar mass star

Jan 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991apj...367..228r&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 367, Jan. 20, 1991, p. 228-238.

Astronomy and Astrophysics

Astrophysics

54

Neutrons, Nuclear Astrophysics, Nuclear Capture, Nuclear Fusion, Stellar Evolution, Stellar Mass, Asymptotic Giant Branch Stars, Reaction Kinetics, Solar System

Scientific paper

Evolutionary calculations of a typical massive star are run in order to analyze the n-capture process occurring during the hydrostatic core He-burning phase, studying the effects of variations in the C-12(alpha, gamma)O-16 and Ne-22(alpha, n)Mg-25 rates within their present uncertainties and in other nuclear inputs. The nucleosynthetic mechanism is characterized by a low mean neutron density, which never exceeds 10 to the 6th n/cu cm. A good production of the s-isotopes in the atomic mass range 70-90 is found, the actual neutron exposure depending on some critical parameters. Important contributions are also found for several light n-rich species and for the heavy rare isotopes Gd-152 and Ta-180. How s-processing in a typical massive star compares with predictions by classical analysis is addressed.

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