Abstract
We follow the chemical evolution of the solar neighbourhood (the elements He, C, N, O, Ne, Mg, Si, S, Ca and Fe) using a galactic chemical evolutionary code that includes the most recent results of single and binary star evolution. First we discuss the differences in the overall net yields produced seperately by binary and single star evolution for different initial metallicities. Then we implement binary evolution into a galactic code that simulates the chemical evolution of the solar neighbourhood as function of time. Our galactic code makes it possible to study the evolution in time of the rate of the different types of supernovae.Keywordsbinariespopulation synthesissupernovaechemical evolution
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