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The recent experimental evaluation of the 18F(a,p)21Ne reaction rate, whenconsidering its associated uncertainties, presented significant differencescompared to the theoretical Hauser-Feshbach rate. This was most apparent at thelow temperatures relevant for He-shell burning in asymptotic giant branch (AGB)stars. Investigations into the effect on AGB nucleosynthesis revealed that theupper limit resulted in an enhanced production of 19F and 21Ne in carbon-richAGB models, but the recommended and lower limits presented no differences fromusing the theoretical rate. This was the case for models spanning a range inmetallicity from solar to [Fe/H] ~ -2.3. The results of this study are relevantfor observations of F and C-enriched AGB stars in the Galaxy, and to the Necomposition of mainstream silicon carbide grains, that supposedly formed in theoutflows of cool, carbon-rich giant stars. We discuss the mechanism thatproduces the extra F and summarize our main findings.

The impact of the 18F(a,p)21Ne reaction on fluorine production in AGB stars