Comparison of Chemical Evolution Models for the Galactic Disk

Abstract

The {\it best} chemical evolution models for the galactic disk computed by different groups with different assumptions are compared with each other and with the observational constraints. Differences and similarities between the models are discussed, emphasizing the importance of testing not only the solar neighbourhood but the whole disk. The history of the metal abundance gradients is found to be very sensitive to the different model assumptions on the star formation and infall rates, and can therefore provide important clues on the disk evolutionary scenario. All the examined models indicate that the deuterium depletion from its primordial abundance to the present one has been at most a factor of 3 and that the stellar nucleosynthesis of some elements (e.g. $^3$He, $^{13}$C and, possibly, $^{18}$O) requires some revisions.