期刊
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF AUSTRALIA
卷 26, 期 3, 页码 153-160出版社
CAMBRIDGE UNIV PRESS
DOI: 10.1071/AS08053
关键词
nuclear reactions, nucleosynthesis, abundances; stars: AGB and post-AGB
资金
- Italian MIUR-PRIN 2006
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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