  We study orbital inclination changes associated with the precession of a
disc-planet system that occurs through gravitational interaction with a binary
companion on an inclined orbit. We investigate whether this scenario can
account for giant planets on close orbits highly inclined to the stellar
equatorial plane. We obtain conditions for maintaining approximate coplanarity
and test them with SPH-simulations. For parameters of interest, the system
undergoes approximate rigid body precession with modest warping while the
planets migrate inwards. Because of pressure forces, disc self-gravity is not
needed to maintain the configuration. We consider a disc and single planet for
different initial inclinations of the binary orbit to the midplane of the
combined system and a system of three planets for which migration leads to
dynamical instability that reorders the planets. As the interaction is
dominated by the time averaged quadrupole component of the binary's perturbing
potential, results for a circular orbit can be scaled to apply to eccentric
orbits. The system responded adiabatically when changes to binary orbital
parameters occurred on time scales exceeding the orbital period. Accordingly
inclination changes are maintained under its slow removal. Thus the scenario
for generating high inclination planetary orbits studied here, is promising.
