Galactic Chemical Evolution of the s Process from AGB Stars

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Contents Vol 26(3)

doi:10.1071/AS08053

Galactic Chemical Evolution of the s Process from AGB Stars

Alessandra Serminato ^A ^D, Roberto Gallino ^A, Claudia Travaglio ^B, Sara Bisterzo ^A, Oscar Straniero ^C

^A Dipartimento di Fisica Generale, Università di Torino, via P. Giuria, 1, 10125 Torino, Italy
^B Osservatorio Astronomico di Torino (INAF), Strada Osservatorio 20, 10025 Pino Torinese, Italy
^C Osservatorio Astronomico di Collurania (INAF), via M. Maggini, Teramo 64100, Italy
^D Corresponding author. Email: ale.wicked.elf@gmail.com





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Publications of the Astronomical Society of Australia 26(3) 153–160 http://dx.doi.org/10.1071/AS08053
Submitted: 25 November 2008 Accepted: 5 August 2009 Published online: 18 September 2009

Abstract

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, abundances — stars: AGB and post-AGB