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We present three dimensional hydrodynamical simulations aimed at studying thedynamical and chemical evolution of the interstellar medium (ISM) in isolateddwarf spheroidal galaxies (dSphs). This evolution is driven by the explosion ofType II and Type Ia supernovae, whose different contribution on both thedynamics and chemical enrichment is taken into account. Radiative losses areeffective in radiating away the huge amount of energy released by SNeexplosions, and the dSph is able to retain most of the gas allowing a longperiod (>2-3 Gyr) of star formation, as usually observed in this kind ofgalaxies. We are able to reproduce the stellar metallicity distributionfunction (MDF) as well as the peculiar chemical properties of stronglyO-depleted stars observed in several dSphs. The model also naturally predictstwo different stellar populations, with an anti-correlation between [Fe/H] andvelocity dispersion, similarly to what observed in the Sculptor and FornaxdSphs. These results derive from the inhomogeneous pollution of the SNe Ia, adistinctive characteristic of our model. We also applied the model to thepeculiar globular cluster (GC) Omega Cen in the hypothesis that it is theremnant of a formerly larger stellar system, possibly a dSph.

About the Chemical Evolution of dSphs (and the peculiar Globular Cluster Omega Cen)