  Recent observations of several protoplanetary discs have found evidence of
departures from flat, circular motion in the inner regions of the disc. One
possible explanation for these observations is a disc warp, which could be
induced by a planet on a misaligned orbit. We present three-dimensional
numerical simulations of the tidal interaction between a protoplanetary disc
and a misaligned planet. For low planet masses we show that our simulations
accurately model the evolution of inclined planet orbit (up to moderate
inclinations). For a planet massive enough to carve a gap, the disc is
separated into two components and the gas interior and exterior to the planet
orbit evolve separately, forming an inner and outer disc. Due to the
inclination of the planet, a warp develops across the planet orbit such that
there is a relative tilt and twist between these discs. We show that when other
parameters are held constant, the relative inclination that develops between
the inner and outer disc depends on the outer radius of the total disc
modelled. For a given disc mass, our results suggest that the observational
relevance of the warp depends more strongly on the mass of the planet rather
than the inclination of the orbit.
