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We present a numerical study of rapid, so‐called type III migration for Jupiter‐sized planets embedded in a protoplanetary disc. We limit ourselves to the case of outward migration, and study in detail its evolution and physics, concentrating on the structure of the corotation and circumplanetary regions, and processes for stopping migration. We also consider the dependence of the migration behaviour on several key parameters. We perform this study using global, two‐dimensional hydrodynamical simulations with adaptive mesh refinement. We find that the outward‐directed type III migration can be started if the initial conditions support the initial average non‐dimensional migration rate bigger than one. Unlike the inward‐directed migration, in the outward migration the migration rate increases due to the growing of the volume of the co‐orbital region. We find the migration to be strongly dependent on the rate of the mass accumulation in the circumplanetary disc, leading to two possible regimes of migration, fast and slow. The structure of the co‐orbital region and the stopping mechanism differs between these two regimes.

Numerical simulations of type III planetary migration – III. Outward migration of massive planets