We present a grid of new models of rotating and non-rotating stars of solar metallicity. Their evolution was followed form the pre-main sequence stage up to core collapse using a 199 isotope network. The evolution and nucleosynthesis was continued through the supernova stage using a 'piston' model [Woosley, S.E, Weaver, T.A., 1995, ApJS, 101, 181] to simulate the explosion. Final isotopic yields are given for 15 and 25 Mȯ stars with different assumptions regarding the mixing efficiency of semiconvection and for rotating and non-rotating stellar models.
- Stellar evolution