Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 1986
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986mnras.223..683m&link_type=abstract
Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 223, Dec. 15, 1986, p. 683-707.
Astronomy and Astrophysics
Astronomy
22
Asymptotic Giant Branch Stars, Giant Stars, Main Sequence Stars, Neutron Sources, Stellar Mass, Abundance, Heavy Elements, Magnetohydrodynamic Flow, Neutron Flux Density, Nuclear Fusion, Stellar Envelopes
Scientific paper
Observations of the heavy-element abundance anomalies in many low-mass giant stars indicate some form of mixing between their envelopes and their interiors. Such mixing could arise following helium-shell flashes on either the AGB or the post-AGB. As a consequence of this mixing a large neutron flux can be produced via the C-12(p, gamma)N-13(beta+ nu)C-13(alpha, n)O-16 sequence of nuclear reactions. As a prerequisite to any model of the heavy-element synthesis which would occur under such a neutron flux, it is important to fully investigate the processes which control neutron production in low-mass AGB and post-AGB stars. It is shown how the ingestion rate of the envelope matter, the effect of intershell splitting and the mixing mechanism adopted can influence the neutron flux. It is found that neutron densities of typically 10 to the 11th neutrons/cu cm and 10 to the 14th neutrons /cu cm are produced from the most likely low-mass AGB mixing and post-AGB mixing event respectively.
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