Abstract
In this work we make use of the Millennium Run, which is at the moment the largest high-resolution simulation of structure formation ever carried out, combined with the semi-analytical model of De Lucia & Blaizot (2007), to follow the chemical evolution of Milky Way type galaxies with the aim at understanding their level of enrichment and the dispersion in the mass-metallicity correlation. Our results suggest that Milky Way type systems tend to evolve passively with time without suffering significant mass accretion. The chemical enrichment of these systems seems to be driven mainly by gas cooling, star formation efficiency and for the most massive progenitors by AGN feedback.
