My research is concerned with fluid models (hydrodynamics, magnetohydrodynamics, and extensions of these concepts). Fluid models can be applied to physics on a huge range of spatial and temporal scales, so that they are the cornerstone of Astrophysical Theory.

My work examines (1) the fluid dynamics (convection, waves, mixing) of the stellar interior, and (2) the plasma dynamics (turbulence, shocks, waves, diffusion) of the interstellar and interplanetary media. I am particularly interested in the interaction of particles and fluids.

What is the deep interior of a star like, and how does their internal structure evolve as they age?

How does a compressible flow interact with stellar convection?

How do we quantify mixing between different layers, deep within a star?

How do magnetic fields grow and become organized?

Have a look at some recent talks I gave: "Realistic global simulations of stellar interiors" Dec 2020.

Pratt, Jane, Baraffe, Isabelle, Dethero, Mary Geer (GSU Student Author), et. al. (2021). Deep mixing due to convective penetration during the red giant branch luminosity bump. Presented at the The 20.5 Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun (CS20.5), virtually anywhere: Zenodo.

How does turbulence change when a magnetic field is present?

How does turbulence change when the flow has a preferred direction?

How do dust particles and cosmic rays disperse in a turbulent plasma?

How does compressibility change diffusion and dispersion in a turbulent plasma?

Can we develop statistical tools to help quantify and predict turbulence?