Milky Way chemo-dynamics in the era of Gaia
  The main goal of Galactic Archaeology is understanding the formation and
evolution of the basic Galactic components. This requires sophisticated
chemo-dynamical modeling, where disc asymmetries (e.g., perturbations from the
central bar, spirals arms, and infalling satellites) and non-equilibrium
processes are taken into account self-consistently. Here we discuss the current
status of Galactic chemo-dynamical modeling and focus on a recent hybrid
technique, which helps circumvent traditional problems with chemical enrichment
and star formation encountered in fully self-consistent cosmological
simulations. We show that this model can account for a number of
chemo-kinematic relations in the Milky Way. In addition, we demonstrate that
(1) our model matches well the observed age-[alpha/Fe] and age-[Fe/H] relations
and (2) that the scatter in the age-[Fe/H] relation cannot be simply explained
by blurring (stars on apo- and pericenters visiting the solar vicinity) but
significant radial migration (stars born elsewhere but ending up at the solar
vicinity today because of a change in guiding radius) is needed. We emphasize
the importance of accurate stellar ages, such as those obtained through
asteroseismology by the CoRoT and Kepler missions, for breaking the degeneracy
among different Galactic evolution scenarios.
