The s Process: Nuclear Physics, Stellar Models, Observations

Details The s Process: Nuclear Physics, Stellar Models, Observations The s Process: Nuclear Physics, Stellar Models, Observations

2010-12-23

arxiv.org/abs/1012.5218v1

Astronomy and Astrophysics

Astrophysics

Solar and Stellar Astrophysics

53 pages, 20 figures, 3 tables; Reviews of Modern Physics, accepted

Scientific paper

Nucleosynthesis in the s process takes place in the He burning layers of low mass AGB stars and during the He and C burning phases of massive stars. The s process contributes about half of the element abundances between Cu and Bi in solar system material. Depending on stellar mass and metallicity the resulting s-abundance patterns exhibit characteristic features, which provide comprehensive information for our understanding of the stellar life cycle and for the chemical evolution of galaxies. The rapidly growing body of detailed abundance observations, in particular for AGB and post-AGB stars, for objects in binary systems, and for the very faint metal-poor population represents exciting challenges and constraints for stellar model calculations. Based on updated and improved nuclear physics data for the s-process reaction network, current models are aiming at ab initio solution for the stellar physics related to convection and mixing processes. Progress in the intimately related areas of observations, nuclear and atomic physics, and stellar modeling is reviewed and the corresponding interplay is illustrated by the general abundance patterns of the elements beyond iron and by the effect of sensitive branching points along the s-process path. The strong variations of the s-process efficiency with metallicity bear also interesting consequences for Galactic chemical evolution.

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