Rotationally constrained convection in extreme parameter regimes

Buoyantly driven convection under the strong influence of rotation is a ubiquitous feature of geophysical and astrophysical fluid flows. It is known to be a principal ingredient in the generation of observable large-scale shear flows and magnetic fields within planetary and stellar interiors. The constraint of geostrophy, the dominant force balance between the pressure gradient force and the Coriolis force, is known to be prevalent and responsible for introducing strong spatial anisotropy that greatly impacts the global circulations, and the energy and momentum transport properties of a rotating fluid. Quasi-Geostrophy, the flow evolution of a rotating fluid under geostrophic constraint, has been a well-developed staple of geophysical fluid dynamics for stably-stratified atmospheric and oceanic flows. The case for QG convectively unstably environments is a far more open research branch. In this talk, I will describe progress in understanding rotating convection through the development of asymptotically reduced models. The canonical paradigm of rapidly rotating Rayleigh-Benard thermal convection will be a specific focus. I will discuss how synergistic efforts asymptotic theory, laboratory and numerical simulations are advancing our understanding of rotating convective flows that include ever greater geophysical and astrophysical complexity.