Internal gravity waves in magnetic stars

Internal gravity waves (or g-modes) propagate in the radiation zones of stars, such as in the radiative core of the Sun. These waves can be excited in stars by turbulence in neighbouring convection zones, by fluid instabilities, or by gravitational tidal forcing due to a companion, such as a closely orbiting hot Jupiter. Stars such as the Sun are magnetised objects. For example, the solar radiation zone is believed to harbour a large-scale magnetic field, which is thought to explain the approximate solid body rotation of the core. However, the effects of magnetic fields on the propagation of gravity waves, and on their stability and dissipation has not been fully explored. This theoretical and computational project will focus on studying aspects of the effects of magnetic fields on gravity waves in stellar and planetary interiors. The goal is to understand the effects of magnetic fields on these waves, and to determine any astrophysical implications for gravity waves that are tidally-excited in exoplanet or close binary systems, as well as the in cores of red giant stars.