Nucleosynthesis in asymptotic giant branch stars: Relevance for Galactic enrichment and solar system formation

We present a review of nucleosynthesis in AGE stars outlining the development of theoretical models and their relationship to observations. We focus on the new high resolution codes with improved opacities, which recently succeeded in accounting for the third dredge-up. This opens the possibility of understanding low luminosity C stars (enriched in s-elements) as the normal outcome of AGE evolution, characterized by production of C-12 and neutron-rich nuclei in the He intershell and by mass loss from strong stellar winds. Neutron captures in AGE stars are driven by two reactions: C-13(alpha,n)O-16, which provides the bulk of the neutron flux at low neutron densities (N-n less than or equal to 10(7) n/cm(3)), and Ne-22(alpha,n)Mg-25, which is mildly activated at higher temperatures and mainly affects the production of s-nuclei depending on reaction branchings. The first reaction is now known to occur in the radiative interpulse phase, immediately below the region previously homogenized by third dredge-up. The second reaction occurs during the convective thermal pulses. The resulting nucleosynthesis phenomena are rather complex and rule out any analytical approximation (exponential distribution of neutron fluences). Nucleosynthesis in AGE stars, modeled at different metallicities, account for several observational constraints, coming from a wide spectrum of sources: evolved red giants rich in s-elements, unevolved stars at different metallicities, presolar grains recovered from meteorites, and the abundances of s-process isotopes in the solar system. In particular, a good reproduction of the solar system main component is obtained as a result of Galactic chemical evolution that mixes the outputs of AGE stars of different stellar generations, born with different metallicities and producing different patterns of s-process nuclei. The main solar s-process pattern is thus not considered to be the result of a standard archetypal s-process occurring in all stars. Concerning the C-13 neutron source, its synthesis requires penetration of small amounts of protons below the convective envelope, where they are captured by the abundant C-12 forming a C-13-rich pocket. This penetration cannot be modeled in current evolutionary codes, but is treated as a free parameter. Future hydrodynamical studies of time dependent mixing will be required to attack this problem. Evidence of other insufficiencies in the current mixing algorithms is common throughout the evolution of low and intermediate mass stars, as is shown by the inadequacy of stellar models in reproducing the observations of CNO isotopes in red giants and in circumstellar dust grains. These observations require some circulation of matter between the bottom of convective envelopes and regions close to the ii-burning shell (cool bottom processing). AGE stars are also discussed in the light of their possible contribution to the inventory of short-lived radioactivities that were found to be alive in the early solar system. We show that the pollution of the protosolar nebula by a close-by AGE star may account for concordant abundances of Al-26, Ca-41 Fe-60, and Pd-107. The AGE star must have undergone a very small neutron exposure, and be of small initial mass (M less than or equal to 1.5 M-.) There is a shortage of Al-26 in such models, that however remains within the large uncertainties of crucial reaction rates. The net Al-26 production problem requires further investigation.