We have developed a detailed standard chemical evolution model to study the evolution of all the chemical 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 \sim 1 Gyr , the halo and the thick disk were assembled out of primordial gas , while the thin disk formed in a second episode of infall of slightly enriched extragalactic gas , with much longer timescale .
The model nicely reproduces the main observational constraints of the solar neighborhood , and the calculated 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 isotopes 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 .