Chemical Evolution of Dwarf Spheroidal and Blue Compact Galaxies

We studied the chemical evolution of Dwarf Spheroidal (dSph) and Blue Compact Galaxies (BCGs) by means of comparison between the predictions of chemical evolution models and several observed abundance ratios. Detailed models with up to date nucleosynthesis taking into account the role played by supernovae of different types (II, Ia) were developed for both types of galaxies allowing us to follow the evolution of several chemical elements. The models are specified by the prescriptions of the star formation (SF) and galactic wind efficiencies chosen to reproduce the main features of these galaxies. We also investigated a possible connection in the evolution of dSph and BCGs and compared the predictions of the models to the abundance ratios observed in Damped Lyman alpha Systems (DLAs). The main conclusions are: i) the observed distribution of [alpha/Fe] vs. [Fe/H] in dSph is mainly a result of the SF rate coupled with the wind efficiency; ii) a low SF efficiency and a high wind efficiency are required to reproduce the observational data for dSph; iii) the low gas content of these galaxies is the result of the combined action of gas consumption by SF and gas removal by galactic winds; iv) the BCGs abundance ratios are reproduced by models with 2 to 7 bursts of SF with low efficiencies ; v) the low values of N/O observed in BCGs are the natural result of a bursting SF; vi) a connection between dSph and BCGs in an unified evolutionary scenario is unlikely; vii) the models for the dSph and BCGs imply different formation scenarios for the DLAs; viii) a suitable amount of primary N produced in massive stars can be perhaps an explanation for the low plateau in the [N/$\alpha$] distribution observed in DLAs, if real.