Modelling the balance of forces in planets and stars

Many planets and stars have self-sustaining magnetic fields generated by 'dynamo action'. This process occurs within a fluid region (e.g. Earth's liquid iron outer core, the solar convection zone, and planetary atmospheres).

The research proposed in this project is primarily motivated by a desire to better understand the fluid dynamics - including convection processes - and magnetic field generation - the 'dynamo process' - within planets and stars. Such systems are governed by a set of complex partial differential equations governing the fluid velocity, magnetic field strength, and energy.

Numerical simulations of these equations are used to provide insight into the dynamics of the chaotic fluid regions where magnetic fields are generated.

This project will involve working with existing numerical code to perform simulations and data analysis of results. The importance of different forces in the governing equations (e.g. Coriolis, Lorentz, viscous forces) determine the dynamics, the dynamo regime, and hence the morphology and strength of the magnetic field that is produced.

The aim of the project will be to improve understanding of how the 'balance of forces' varies spatially and differs across parameter regimes. This would allow identification of the dynamo regimes most appropriate for planets and stars.