  In chemodynamical evolution models it is usually assumed that the Milky Way
galaxy forms from the inside-out implying that gas inflows onto the disk
decrease with galactocentric distance. Similarly, to reproduce differences
between chemical abundances of the thick disk and bulge with respect to those
of the thin disk, higher accretion fluxes at early times are postulated. By
using a suite of Milky Way-like galaxies extracted from cosmological
simulations, we investigate the accretion of gas on the simulated stellar disks
during their whole evolution. In general, we find that the picture outlined
above holds, although the detailed behavior depends on the assembly history of
the Galaxy and the complexities inherent to the physics of galaxy formation.
