  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 co-rotation 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 $Z > 1$, that corresponds to initial value
$M_\rmn{\Delta} \ga 1.5$. 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 differ between these two regimes.
