We present a new method that allows for long-term and large-scale hydrodynamical simulations of migrating planets over a grid-based Eulerian code. This technique, which consists of a remapping of the disk by tracking the planetary migration, enables runs of migrating planets over a time comparable to the age of protoplanetary disks. This method also has the potential to address efficiency problems related to the migration of multi-planet systems in gaseous disks and to improve the current results of the migration of massive planets by including global viscous evolution as well as detailed studies of the co-orbital region during migration. We perform different tests using the public code FARGO3D to validate this method and compare its results with those obtained using a classical fixed grid.
- methods: numerical
- planet-disk interactions