Neutron-capture nucleosynthesis in AGB stars

Recent AGE models including diffusive overshoot or rotational effects sugge st the partial mixing (PM) of protons from the H-rich envelope into the C-r ich layers during the third dredge-up. In order to study the impact of such a mixing on the surface abundances, nucleosynthesis calculations based on stellar AGE models are pet-formed for different assumptions of protons (ran ging from X-p(mix) = 10(-6) to 0.7) in the PM zone. For high proton-to-C-12 abundance ratios, light nuclei such as fluorine and sodium are efficiently produced, while heavier s-process nuclei are synthesized for lower proton- to-C-12 ratios. In the framework of the PM model, assuming a smooth exponentially decreasin g proton profile? the surface F-19 abundance evolution is correlated with t hat of s-process nuclei in agreement with observations. However, as a funct ion of the surface C/O abundance ratio, the surface F-19 enrichment remains difficult to reconcile with observations in AGE stars. Sodium is predicted to be efficiently produced in a small region of the Phl zone with proton-t o-C-12 abundance ratio of about 10, but with large overproduction factors ( up to fifty times higher than the sodium left over by the hydrogen burning shell). The primary C-13 pocket formed in the PM zone at low proton-to-C-12 ratios is responsible for an efficient production of s-process nuclei. A table of elemental overabundances predicted at the surface of AGE stars at four diff erent metallicities is presented. All the nucleosynthesis calculations are shown to suffer from major nuclear reaction rate uncertainties, in particular, C-13(p, gamma) N-14, N-14(n, p ) C-14 and Ne-22(alpha, n) Mg-25. The major uncertainties associated with t he amount of protons mixed into the C-rich zone are found in the extent of the PM zone rather than in the adopted H profile. Finally, the PM scenario predicts that low-metallicity AGE stars enriched i n s-process elements should exhibit a large overproduction of Pb and Bi com pared to other s-isotopes. The search of such Pb-stars is highly encouraged .