Correlated nucleosynthesis of fluorine and s-process elements in asymptotic giant branch stars

Details Correlated nucleosynthesis of fluorine and s-process elements in asymptotic giant branch stars Correlated nucleosynthesis of fluorine and s-process elements in asymptotic giant branch stars

Jun 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998a%26a...334..153m&link_type=abstract

Astronomy and Astrophysics, v.334, p.153-158 (1998)

Astronomy and Astrophysics

Astrophysics

25

Nucleosynthesis, Stars: Abundances, Stars: Agb

Scientific paper

The production of fluorine and s-process elements in conditions simulating the helium-burning shell of asymptotic giant branch (AGB) stars is investigated from parametric one-zone nucleosynthesis calculations. Our calculations account for the correlation between the overabundances of these elements, as observed at the surface of S and C stars (Jorissen et al. 1992, A&A 261, 164). A primary supply of \chem{C}{13} is, however, required to produce \chem{F}{19} and s-process elements at the observed levels through the operation of the \chem{C}{13}(alpha ,n)\chem{O}{16} neutron source. Our calculations allow to put strong constraints on this primary supply. They require a \chem{C}{13} mass fraction of at least 0.003, with little sensitivity to the stellar conditions. This value is about 30 times larger than the secondary \chem{C}{13} supply available at the end of the CNO cycle in solar-metallicity stars. The minimum \chem{N}{14} mass fractions required are found to vary between about 6; 10(-4) and 0.01, depending on the temperature at which the fluorine production occurs.

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