出版社：SISSA, Scuola Internazionale Superiore di Studi Avanzati
摘要：The recent experimental evaluation of the 18F(a,p)21Ne reaction rate, when considering its associated
uncertainties, presented significant differences compared to the theoretical Hauser-Feshbach
rate. This was most apparent at the low temperatures relevant for He-shell burning in asymptotic
giant branch (AGB) stars. Investigations into the effect on AGB nucleosynthesis revealed that the
upper limit resulted in an enhanced production of 19F and 21Ne in carbon-rich AGB models, but
the recommended and lower limits presented no differences from using the theoretical rate. This
was the case for models spanning a range in metallicity from solar to [Fe/H] ∼ −2.3. The results
of this study are relevant for observations of F and C-enriched AGB stars in the Galaxy, and to the
Ne composition of mainstream silicon carbide grains, that supposedly formed in the outflows of
cool, carbon-rich giant stars. We discuss the mechanism that produces the extra F and summarize
our main findings.
