A chemical evolution model in which nucleosynthesis products coming from type I and II SNe are taken into account is presently used to compute the evolution of C-12, O-16, Mg-24, Si-28, and Fe-56 in the solar neighborhood. A binary model is used for the type I SNe, and a detailed rate of their occurrence is obtained. Attention is given to the implications of the good reproduction obtained for the behavior of the O/Fe abundance ratio in both halo and disk stars. Overabundances of Si and Mg are predicted for metal-poor stars; the finding that C should be overabundant in metal-poor stars, at variance with the observations, is suggested to be due to either a too-high Fe production from type I SNe or to a need for the theoretical yield of C from type II SNe to be smaller.
