  It has been suggested that tidal interaction is important for shaping the
orbital configurations of close orbiting giant planets. The excitation of
propagating waves and normal modes (dynamical tide) will be important for
estimating time scales for orbital evolution. We consider the tidal interaction
of a Jupiter mass planet orbiting a solar type primary. Tidal and rotational
frequencies are assumed comparable making the effect of rotation important.
Although centrifugal distortion is neglected, Coriolis forces are fully taken
into account. We focus in detail on the potentially resonant excitation of $r$
modes associated with spherical harmonics of degrees three and five. These are
mostly sited in the radiative core but with a significant response in the
convective envelope where dissipation occurs. Away from resonance significant
orbital evolution over the system lifetime is unlikely. However, tidal
interaction is enhanced near resonances and the orbital evolution accelerated
as they are passed through. This speed up may be sustained if near resonance
can be maintained. For close orbits with primaries rotating sufficiently
rapidly, this could arise from angular momentum loss and stellar spin down
through a stellar wind bringing about significant orbital evolution over the
system lifetime.
