  We calculate the conversion from non-adiabatic, non-radial oscillations
tidally induced by a hot Jupiter on a star to observable spectroscopic and
photometric signals. Models with both frozen convection and an approximation
for a perturbation to the convective flux are discussed. Observables are
calculated for some real planetary systems to give specific predictions.
Time-dependent line broadening and the radial velocity signal during transit
are both investigated as methods to provide further insight into the nature of
the stellar oscillations. The photometric signal is predicted to be
proportional to the inverse square of the orbital period, $P^{-2}$, as in the
equilibrium tide approximation. However, the radial velocity signal is
predicted to be proportional to $ P^{-1}$, and is therefore much larger at long
orbital periods than the signal corresponding to the equilibrium tide
approximation, which is proportional to $P^{-3}$. The prospects for detecting
these oscillations and the implications for the detection and characterisation
of planets are discussed.
