Stellar Oscillations Tidally Induced by a Planetary Companion
The tidal potential due to a close-in, massive planet such as a Hot Jupiter drives non-radial stellar oscillations causing periodic fluctuations in both the radiative flux and radius of the star. These could be potentially detected in the form of variations in luminosity, wavelength, or lineshape of the star's light. I have modelled these oscillations using the Henyey method to solve the non-adiabatic oscillation equations, and have calculated their observational signals in terms of both spectroscopy and photometry.
Potential prospects for the successful application of this technique include breaking the mass-inclination degeneracy in RV detections, using photometry to detect non-transiting planets, and removing second-order effects from Hot Jupiters in order to improve the possibility of detecting other planets in the system.