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We study the role of radial migration of stars on the chemical evolution ofthe Milky Way disk. In particular, we are interested in the impact of thatprocess on the local properties of the disk (age-metallicity relation and itsdispersion, metallicity distribution, evolution of abundance ratios) and on themorphological properties of the resulting thick and thin disks.We use a modelwith several new or up-dated ingredients: atomic and molecular gas phases, starformation depending on molecular gas, yields from the recent homogeneous gridprovided by Nomoto et al. (2013), observationally inferred SNIa rates. Wedescribe radial migration with parametrised time- and radius-dependentdiffusion coefficients, based on the analysis of a N-body+SPH simulation. Wealso consider parametrised radial gas flows, induced by the action of theGalactic bar. Our model reproduces well the present day values of most of themain global observables of the MW disk and bulge, and also the observed"stacked" evolution of MW-type galaxies from van Dokkum et al. (2013). Theazimuthally averaged radial velocity of gas inflow is constrained to less thana few tenths of km/s. Radial migration is constrained by the observeddispersion in the age-metallicity relation. Assuming that the thick disk is theoldest (>9 Gyr) part of the disk, we find that the adopted radial migrationscheme can reproduce quantitatively the main local properties of the thin andthick disk. The thick disk extends up to ~11 kpc and has a scale length of 1.8kpc, considerably shorter than the thin disk, because of the inside-outformation scheme. We also show how, in this framework, current and forthcomingspectroscopic observations can constrain the nucleosynthesis yields of massivestars for the metallicity range of 0.1 solar to 2-3 solar.

Evolution of the Milky Way with radial motions of stars and gas I. The solar neighborhood and the thin and thick disk