The s process: Nuclear physics, stellar models, and observations
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In this article, the authors present a review of the state-of-the-art in the area of observations, nuclear and atomic physics, and stellar modeling, 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.Abstract:
Nucleosynthesis in the $s$ process takes place in the He-burning layers of low-mass asymptotic giant branch (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 an 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.read more
Citations
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Core-Collapse Supernovae from 9 to 120 Solar Masses Based on Neutrino-powered Explosions
TL;DR: In this paper, a grid of supernovae resulting from massive stars with solar metallicity and masses from 9.0 to 120 solar masses are calculated for nucleosynthesis, light curves, explosion energies, and remnant masses.
Journal ArticleDOI
Nucleosynthesis in Stars and the Chemical Enrichment of Galaxies
TL;DR: In this article, the authors review the recent results of the nucleosynthesis yields of mainly massive stars for a wide range of stellar masses, metallicities, and explosion energies, and provide yields tables and examine how those yields are affected by some hydrodynamical effe...
Journal ArticleDOI
Core-Collapse Supernovae from 9 to 120 Solar Masses Based on Neutrino-powered Explosions
TL;DR: In this paper, a grid of supernovae resulting from massive stars with solar metallicity and masses from 9.0 to 120 solar masses are calculated for nucleosynthesis, light curves, explosion energies, and remnant masses.
s-process nucleosynthesis-nuclear physics and the classical model
F. Käppeler,H. Beer,K. Wisshak +2 more
TL;DR: In this article, the status of this classical approach is reviewed with emphasis on the implications for various stellar models of the s-process and in the light of results obtained by stellar spectroscopy.
Journal ArticleDOI
The impact of individual nuclear properties on $r$-process nucleosynthesis
TL;DR: A review of recent sensitivity studies of the rapid neutron capture process can be found in this article, which summarizes the extent of such sensitivity studies and highlights how these studies play a key role in facilitating new insight into the r-process nucleosynthesis.
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