  I present a review of chemical evolution models of the solar neighborhood. I
give special attention to the necessary ingredients 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 chemical evolution models that reach
super-solar metallicities is the computation of stellar yields for stellar
metallicities higher than the initial solar value. Based on 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 with the
initial solar abundances.
