  The unusual spectral energy distribution (SED) of the classical T Tauri star
GM Aurigae provides evidence for the presence of an inner disc hole extending
to several au. Using a combination of hydrodynamical simulations and Monte
Carlo radiative transport, we investigate whether the observed SED is
consistent with the inner hole being created and maintained by an orbiting
planet. We show that an ~ 2 M_Jupiter planet, orbiting at 2.5 au in a disc with
mass 0.047 M_sun and radius 300 au, provides a good match both to the SED and
to CO observations which constrain the velocity field in the disc. A range of
planet masses is allowed by current data, but could in principle be
distinguished with further observations between 3 and ~ 20 microns. Future high
precision astrometric instruments should also be able to detect the motion of
the central star due to an orbiting Jupiter mass planet. We argue that the
small number of T Tauri stars with SEDs resembling that of GM Aur is broadly
consistent with the expected statistics of embedded migrating planets.
