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Elliptical galaxies probably host the most metal rich stellar populations inthe Universe. The processes leading to both the formation and the evolution ofsuch stars are discussed by means of a new gas dynamical model which implementsdetailed chemical evolution prescriptions. Moreover, the radial variations inthe metallicity distribution of these stars are investigated by means ofG-dwarf-like diagrams. By comparing model predictions with observations, wederive a picture of galaxy formation in which the higher is the mass of thegalaxy, the shorter are the infall and the star formation timescales. Thegalaxies seem to have formed outside-in, namely the most external regionsaccrete gas, form stars and develop a galactic wind very quickly (a few Myr)compared to the central core, where the star formation can last up to 1 Gyr. Weshow for the first time a model able in reproducing the mass-metallicity andthe color-magnitude relations as well as the radial metallicity gradient, and,at the same time, the observed either positive or negative slopes in the[alpha/Fe] abundace ratio gradient in stars.

What hydrodynamical simulations tell us about the radial properties of the stellar populations in Ellipticals