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Published online by Cambridge University Press: 02 December 2009
I present a review of chemical-evolution models of the Solar neighborhood. I pay special attention to the ingredients necessary to reproduce the observed [Xi/Fe] ratios in nearby metal- and super-metal-rich stars, and to the chemical properties of the Solar vicinity, focusing on [Fe/H]≥–0.1. I suggest that the observed abundance trends are due to material synthesized and ejected by intermediate-mass stars with Solar metallicity in the AGB stage, and also by massive stars with (super)solar metallicity in the stellar wind and supernovae stages. The required tool to build chemicalevolution models that reach supersolar metallicities is the computation of stellar yields for stellar metallicities higher than the initial Solar value. With these models it might be possible to estimate the importance of merger events in the recent history of the Galactic disk as well as the relevance of radial stellar migration from the inner to the outer regions of the Galaxy. I also present a short review of the photospheric Solar abundances and their relation to the initial Solar abundances.
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