  We study the role of radial motions of stars and gas on the evolution of
abundance profiles in the Milky Way disk. We investigate, in a parametrized
way, the impact of radial flows of gas and radial migration of stars induced
mainly by the Galactic bar and its iteraction with the spiral arms. We use a
model with several new or up-dated ingredients (atomic and molecular gas
phases, star formation depending on molecular gas, recent sets of
metallicity-dependent stellar yields from H to Ni, observationally inferred
SNIa rates), which reproduces well most global and local observables of the
Milky Way. We obtain abundance profiles flattening both in the inner disk
(because of radial flows) and in the outer disk (because of the adopted star
formation law). The gas abundance profiles flatten with time, but the
corresponding stellar profiles appear to be steeper for younger stars, because
of radial migration. We find a correlation between the stellar abundance
profiles and O/Fe, which is a proxy for stellar age. Our final abundance
profiles are in overall agreement with observations, but slightly steeper (by
0.01-0.02 dex/kpc) for elements above S. We find an interesting "odd-even
effect" in the behaviour of the abundance profiles (steeper slopes for odd
elements) for all sets of stellar yields; however, this behaviour does not
appear in observations, suggesting that the effect is, perhaps, overestimated
in current stellar nucleosynthesis calculations.
