Estimating the actual stellar diffusion in a barred spiral
Maura Brunetti, Cristina Chiappini
We characterize empirically the radial diffusion of stars in a typical barred disk galaxy by calculating the local spatial diffusion coefficient and diffusion time-scale for bulge-disk-halo N-body self-consistent systems which differ initially on the Safronov-Toomre-Q parameter. We find that different diffusion scenarios appear depending on the bar strength and on the degree of stability of the disk. Marginally stable disks, with Q~1, have two families of bar orbits with different values of angular momentum and energy, which determine a large diffusion in the corotation region. In hot disks (Q>1) stellar diffusion is reduced with respect to the case of marginally stable disks. For all models the spatial diffusion is not constant in time and depends on the activity of the bar, which can move stars all over the disk recurrently. To realistically study the impact of radial migration on chemical evolution modeling of the Milky Way, the role of its bar has to be taken into account.