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Galactic Chemical Evolution of the s Process from AGB Stars

Published online by Cambridge University Press:  05 March 2013

Alessandra Serminato ,
Roberto Gallino ,
Claudia Travaglio ,
Sara Bisterzo  and
Oscar Straniero
Alessandra Serminato*
Affiliation:
Dipartimento di Fisica Generale, Università di Torino, via P. Giuria, 1, 10125 Torino, Italy
Roberto Gallino
Affiliation:
Dipartimento di Fisica Generale, Università di Torino, via P. Giuria, 1, 10125 Torino, Italy
Claudia Travaglio
Affiliation:
Osservatorio Astronomico di Torino (INAF), Strada Osservatorio 20, 10025 Pino Torinese, Italy
Sara Bisterzo
Affiliation:
Dipartimento di Fisica Generale, Università di Torino, via P. Giuria, 1, 10125 Torino, Italy
Oscar Straniero
Affiliation:
Osservatorio Astronomico di Collurania (INAF), via M. Maggini, Teramo 64100, Italy
*
DCorresponding author. Email: ale.wicked.elf@gmail.com
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Abstract

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We follow the chemical evolution of the Galaxy for the s elements using a Galactic chemical evolution (GCE) model, as already discussed by Travaglio et al. (1999, 2001, 2004), with a full updated network and refined asymptotic giant branch (AGB) models. Calculations of the s contribution to each isotope at the epoch of the formation of the solar system is determined by following the GCE contribution by AGB stars only. Then, using the r-process residual method we determine for each isotope their solar system r-process fraction, and recalculate the GCE contribution of heavy elements accounting for both the s and r process. We compare our results with spectroscopic abundances at various metallicities of [Sr,Y,Zr/Fe], of [Ba,La/Fe], of [Pb/Fe], typical of the three s-process peaks, as well as of [Eu/Fe], which in turn is a typical r-process element. Analysis of the various uncertainties involved in these calculations are discussed.

Keywords

nuclear reactions, nucleosynthesis, abundancesstars: AGB and post-AGB
Type
Theory, Evolution and Models
Information
Publications of the Astronomical Society of Australia , Volume 26 , Issue 3 , 2009 , pp. 153 - 160
Copyright
Copyright © Astronomical Society of Australia 2009

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