Galactic Chemical Evolution of the s Process from AGB Stars

Publications of the Astronomical Society of Australia

Alessandra Serminato¹ 

[1] Roberto Gallino

关键词: nuclear reactions;    nucleosynthesis;    abundances;    stars: AGB and post-AGB;   

DOI  :  10.1071/AS08053

学科分类：天文学(综合)

来源: CSIRO

【 摘 要 】

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.

【 授权许可】

Unknown