Oxygen, Carbon and Nitrogen evolution in galaxies

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Abstract
We discuss the evolution of oxygen, carbon and nitrogen in galaxies of different morphological type by adopting detailed chemical evolution models with different star formation histories (continuous star formation or starbursts). We start by computing chemical evolution models for the Milky Way with different stellar nucleosynthesis prescriptions. Then, a comparison between model results and ``key'' observational constraints allows us to choose the best set of stellar yields. Once the best set of yields is identified for the Milky Way, we apply the same nucleosynthesis prescriptions to other spirals (in particular M101) and dwarf irregular galaxies. We compare our model predictions with the [C,N,O/Fe] vs. [Fe/H], log(C/O) vs. 12+ log(O/H), log(N/O) vs. 12+ log(O/H) and [C/O] vs. [Fe/H] relations observed in the solar vicinity, along the disk and in other galaxies. By taking into account the results obtained for all the studied galaxies (Milky Way, M101, dwarf galaxies and DLAs) our main conclusions are: a) once the available observational data are properly interpreted, there is no compelling evidence for requiring the production of primary N in massive stars (M>10Msun); b) both C and N we see today in the ISM come mainly from low- and intermediate-mass stars. In particular, there is no need to invoke strong stellar winds in massive stars in order to explain the evolution of C/O ratio in the solar neighborhood, as often claimed in the literature (abridged).

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