  We investigate outflows driven by a giant protoplanet using three-dimensional
MHD nested grid simulations. We consider a local region around the protoplanet
in the protoplanetary disk, and calculate three models: (a) unmagnetized disk
model, (b) magnetized disk model having magnetic field azimuthally parallel to
the disk, and (c) magnetic field perpendicular to the disk. Outflows with
velocities, at least, 10 km/s are driven by the protoplanets in both magnetized
disk models, while outflow does not appear in unmagnetized disk model.
Tube-like outflows along the azimuthal direction of the protoplanetary disk
appear in model with magnetic field being parallel to the disk. In this model,
the magnetically dominated regions (i.e., density gap) are clearly contrasted
from other regions and spiral waves appear near the protoplanet. On the other
hand, in model with magnetic field being perpendicular to the disk, outflows
are driven by a protoplanet with cone-like structure just as seen in the
outflow driven by a protostar. Magnetic field lines are strongly twisted near
the protoplanet and the outflows have well-collimated structures in this
model.These outflows can be landmarks for searching exo-protoplanets in their
formation stages. Our results indicate that the accretion rate onto the
protoplanet tend to have a larger value than that expected from previous
hydrodynamical calculations, since a fraction of the angular momentum of
circum-planetary disk is removed by outflows, enhanced non-axisymmetric
patterns caused by magnetic field, and magnetic braking. Possible implications
for observation are also briefly discussed.
