Galactic Chemical Evolution of the s Process from AGB Stars

Details Galactic Chemical Evolution of the s Process from AGB Stars Galactic Chemical Evolution of the s Process from AGB Stars

2009-09-30

arxiv.org/abs/0909.5570v1

PASA 2009 Volume 26 Number 3, pp. 153-160

Astronomy and Astrophysics

Astrophysics

Solar and Stellar Astrophysics

8 pages, 6 figures, 1 table

Scientific paper

10.1071/AS08053

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.

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