Algorithms for neutron density and s-process nucleosynthesis in a low-mass asymptotic giant branch star

Details Algorithms for neutron density and s-process nucleosynthesis in a low-mass asymptotic giant branch star Algorithms for neutron density and s-process nucleosynthesis in a low-mass asymptotic giant branch star

Jan 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...349..208h&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 349, Jan. 20, 1990, p. 208-221.

Statistics

Computation

25

Asymptotic Giant Branch Stars, Computational Astrophysics, Neutrons, Nuclear Astrophysics, Nuclear Fusion, Particle Flux Density, Capture Effect, Stellar Envelopes, Stellar Interiors, Stellar Models

Scientific paper

Algorithms for calculating neutron-capture nucleosynthesis in the context of low-mass AGB astars are presented. The primary neutron source is the (C-13)(alpha, n) O-16 reaction which is activated in the convective shell of an AGB star having the characteristics found in stellar model calculations. It is shown that a one-zone model is useful for obtaining estimates of the consequence of neutron-capture nucleosynthesis; for a typical pulse, this zone has a temperature of about 1.36 x 10 to the 8th K and a density of about 34,400 g/cu cm. This compares with a temperature of 1.50 x 10 to the 8th K and a density of 40,000 g/cu cm at the base of the convective shell. Each neutron release episode lasts for about 10 yr and, if C-13 is introduced into the convective shell at a constant rate, the mean neutron number density during most of this episode is shown by a given expression.

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