Stellar Radial Migration In Galactic Discs

Abstract

International audienceRadial migration in galactic discs has been more and more studied because of puzzling observations in the Milky Way or local galaxies. Numerical simulations show the migration depends on the parameters of non-axisymmetric patterns (bars or spiral arms). In particular, radial migration may not always be able to cause some observational features of the outer parts of discs. Its impact on the thickness of discs is also debated. We present some results of numerical simulations of isolated galactic discs. Radial migration is studied with respect to the location of the main resonances of the bar of these bar-dominated discs