Part 1 (analysis of stellar migration in AURIGA): Published
Stellar migration in the Auriga simulations

Part 2 (implementation into L-GALAXIES 2020): Ongoing

Periklis Okalidis, Rob Yates, Rob Grand, Volker Springel

Part 1:
We study the presence and importance of stellar migration in the evolution of 17 Milky-Way like disk galaxies with stellar mass 10 < log(M*/M⊙) < 11 from the Auriga suite of zoom-in cosmological hydrodynamical simulations. We compare the birth radii of the stars to their radii at z = 0 for each system and present mean values of the strength of stellar migration as a function of radius and stellar age which vary between 1-4 kpc. We also investigate the effect of migration on age and metallicity radial profiles in the disks. We find several cases of age gradient flattening due to migration, but significant changes to metallicity profiles only for older stellar populations and disks that develop a strong bar. Furthermore, we study stellar migration from the perspective of the change of the galactocentric radius (ΔR) and orbital guiding centre radius (ΔRg) of stellar particles between given time intervals. We find that stars migrate approximately as a diffusion process only in the outer parts of the disks and for particular galaxies that have a weak bar. Strongly barred galaxies in our sample show larger stellar migration but its timestep evolution is slower-than-diffusion. Finally, we give parametrisations that encapsulate the dependence of the strength of the radial migration as a function of time and radius, for incorporation into (semi-)analytic models of galaxy evolution.
Part 2:
The scaling relations produced from the AURIGA analysis above will be implemented into L-Galaxies 2020 and synchronised with the new gas flows recipe which is also being implemented as part of the Radial gas flows in discs project.