出版社：SISSA, Scuola Internazionale Superiore di Studi Avanzati
摘要：Asymptotic Giant Branch stars are the main nuclear production phase of low- and intermediate
mass stars. The double-shell burning of He and H around the electron degenerate core drives a rich
pattern of nucleosynthesis, including the slow neutron capture process, as well as the formation of
neutron rich isotopes. This nucleosynthesis is now observationally accessible in extremely metal
poor stars, in particular the carbon enhanced s- process rich stars in binaries. The most common
approach to model AGB star evolution and nucleosynthesis is the one-dimensional, spherically
symmetric stellar evolution approximation. The input physics (mass loss, convective and nonconvective
mixing, nucleosynthesis) and their uncertainties are discussed. More recently, hydrodynamic
simulations of He-shell flash convection are becoming available, providing the means
for a detailed analysis of some of the uncertain aspects of one-dimensional models. The differences
between stellar interior convection and shallow surface convection is discussed. We also
report on new studies that investigate the sensitivity of mixing and element production to nuclear
reaction rates.
