On s-process nucleosynthesis in thermally pulsing stars

Details On s-process nucleosynthesis in thermally pulsing stars On s-process nucleosynthesis in thermally pulsing stars

Sep 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977apj...216..797t&link_type=abstract

Astrophysical Journal, Part 1, vol. 216, Sept. 15, 1977, p. 797-810.

Astronomy and Astrophysics

Astrophysics

149

Abundance, Late Stars, Nuclear Fusion, Stellar Structure, Thermal Radiation, Enrichment, Heavy Elements, Light Elements, Magnesium Isotopes, Neon Isotopes, Neutron Sources, Tables (Data)

Scientific paper

The detailed operation of s-process nucleosynthesis in the convective shell of a thermally pulsating star is investigated for the case where the Ne-22 (alpha, n) Mg-25 reaction is adopted as a neutron source. A nuclear reaction network extending from Ne-22 to Bi-209 is constructed for tracing the thermonuclear evolution of the matter in the convective shell; the abundances emerging from a 'standard model' that incorporates the relevant properties of detailed models of pulsating stars are found to approach those obtained in the asymptotic limit of a previous approximate calculation. The time variations of the abundance distributions are described, and the number of pulse epochs required for the realization of the asymptotic limiting solutions is determined as a function of the degree of overlap between successive convective shells. Neutron competition from nuclei lighter than iron is discussed together with the associated nucleosynthesis of neutron-rich isotopes in the same atomic-mass range. Analytical expressions exhibiting the controlling features of thermal-pulse neutron exposures are derived, implications of the results for galactic nucleosynthesis are considered, and the s-process distributions estimated for various stellar models are interpreted.

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