Abstract
We have developed a detailed standard chemi- cal evolution model to study the evolution of all the chem- ical elements up to the iron peak in the solar vicinity. We consider that the Galaxy was formed through two episodes of exponentially decreasing infall, out of extragalactic gas. In a first infall episode, with a duration of ∼ 1 Gyr, the halo and the thick disk were assembled out of primordial gas, while the thin disk formed in a second episode of in- fall of slightly enriched extragalactic gas, with much longer timescale. The model nicely reproduces the main observa- tional constraints of the solar neighborhood, and the cal- culated elemental abundances at the time of the solar birth are in excellent agreement with the solar abundances. By the inclusion of metallicity dependent yields for the whole range of stellar masses we follow the evolution of 76 iso- topes of all the chemical elements between hydrogen and zinc. Those results are confronted with a large and recent body of observational data, and we discuss in detail the implications for stellar nucleosynthesis.
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