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We present chemical evolution models of the Galactic disk with differentZ-dependent yields. We find that a moderate mass loss rate for massive stars ofsolar metallicity produces an excellent fit to the observed C/H and C/Ogradients of the Galactic disk. The best model also fits: the H, He, C, and Oabundances derived from recombination lines of M17, the protosolarabundances,and the C/O-O/H, C/Fe-Fe/H, and O/Fe-Fe/H relations derived fromsolar vicinity stars. The agreement of the model with the protosolar abundancesimplies that the Sun originated at a galactocentric distance similar to the oneit has. Our model for $r=3$ kpc implies that a fraction of the stars in thedirection of the bulge formed in the inner disc. We obtain a good agreementbetween our model and the C/O versus O/H relationship derived fromextragalactic H~{\sc ii} regions in spiral galaxies.

HII Regions And the Protosolar Helium, Carbon, and Oxygen Abundances in the Context of Galactic Chemical Evolution