The observed small orbital radii of massive extrasolar planets around
the central solar-type stars can be explained by the mechanisms of
orbital migration. The scenario is: the planet forms in the protoplanetary
disk and induces planet–disk tidal interactions resulting in the
inward migration of the planet. In this thesis, we first construct a onedimensional
disk model corresponding to the observational constraints
and then investigate the effects caused by the embedded planet, including
the regulations of the disk surface density and the planetary
orbital radius. Using numerical simulations, the evolution of the disk
as well as the changes in the planetary orbital radius are produced.
The massive planet (∼ 1MJ ) opens a gap quickly in the vicinity of its
location, and the gap would move with the migrating planet. If the
planet forms earlier in the disk, its extent of migration is larger. We
also find that the more massive planet migrates faster initially, but
the resulting change in orbital radius is not obvious (it would stop
migrating earlier).

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