  Recent spectral observations by the Spitzer Space Telescope (SST) reveal that
some discs around young ($\sim {\rm few} \times 10^6$ yr old) stars have
remarkably sharp transitions to a low density inner region in which much of the
material has been cleared away. It has been recognized that the most plausible
mechanism for the sharp transition at a specific radius is the gravitational
influence of a massive planet. This raises the question of whether the planet
can also account for the hole extending all the way to the star. Using high
resolution numerical simulations, we show that Jupiter-mass planets drive
spiral waves which create holes on time scales $\sim 10$ times shorter than
viscous or planet migration times. We find that the theory of spiral-wave
driven accretion in viscous flows by Takeuchi et al. (1996) can be used to
provide a consistent interpretation of the simulations. In addition, although
the hole surface densities are low, they are finite, allowing mass accretion
toward the star. Our results therefore imply that massive planets can form
extended, sharply bounded spectral holes which can still accommodate
substantial mass accretion rates. The results also imply that holes are more
likely than gaps for Jupiter mass planets around solar mass stars.
