@misc{10481/58393,
year = {2019},
month = {11},
url = {http://hdl.handle.net/10481/58393},
abstract = {The decomposition of the Solar system abundances of heavy isotopes into their sand r- components plays a key role in our understanding of the corresponding nuclear
processes and the physics and evolution of their astrophysical sites. We present a new
method for determining the s- and r- components of the Solar system abundances,
fully consistent with our current understanding of stellar nucleosynthesis and galactic chemical evolution. The method is based on a study of the evolution of the solar
neighborhood with a state-of-the-art 1-zone model, using recent yields of low and intermediate mass stars as well as of massive rotating stars. We compare our results with
previous studies and we provide tables with the isotopic and elemental contributions
of the s- and r-processes to the Solar system composition},
organization = {This article is based upon work partially supported from
the “ChETEC” COST Action (CA16117) of COST (European Cooperation in Science and Technology). C.A. acknowledges in part to the Spanish grants AYA2015-63588-P
and PGC2018-095317-B-C21 within the European Founds
for Regional Development (FEDER).},
publisher = {Oxford University Press},
keywords = {Galaxy},
keywords = {Galaxy: evolution},
keywords = {Nucleosynthesis},
keywords = {Sun: abundances},
title = {Chemical evolution with rotating massive star yields II. A new assessment of the solar s- and r- process components},
author = {Prantzos, N. and Abia, Carlos and Cristallo, S. and Limongi, M. and Chieffi, A.},
}