Tidal waves in stars and planets
- Academic lead
- Prof Adrian J Barker, School of Mathematics, A.J.Barker@leeds.ac.uk
- Co-supervisor(s)
- Dr Stephen Griffiths, School of Mathematics, S.D.Griffiths@leeds.ac.uk, Prof Phil Livermore, School of Earth and Environment, P.W.Livermore@leeds.ac.uk
- Project themes
- Astrophysics & Geophysics, Computational & Analytical Tools
Gravitational tidal forcing excites internal gravity and inertial waves in fluid layers of planets and stars. The dissipation of these waves can produce long-term evolution of the orbits and rotations of stars and planets. For example, hot Jupiters excite internal waves inside the radiative interiors of their host stars, and the dissipation of these waves can cause the planet to spiral inwards and be destroyed within millions to billions of years. To determine the outcome of tidal interactions and make predictions for astronomers, we must improve our understanding of internal and inertial waves. Internal (inertial) waves are fluid waves restored by buoyancy (Coriolis) forces. Despite their different origins, both types of waves share many mathematical properties and can be studied theoretically using similar approaches. This project will analyse the tidal excitation, stability and resulting nonlinear dissipation of inertial and/or internal waves in magnetised, stratified and/or rotating fluids using a combination of analytical and numerical approaches, including direct numerical simulations. Various aspects will be explored during the project, depending on the interests of the student. Results obtained will finally be applied to interpret, and make predictions for, astrophysical observations of extrasolar planets.