2021MNRAS.500.2711B

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. 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 characterization of planets are discussed.