Physics – Fluid Dynamics
Scientific paper
Nov 1998
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998aps..dfd..gi09l&link_type=abstract
American Physical Society, Division of Fluid Dynamics Meeting, November 22-24, 1998 Philadelphia, PA, abstract #GI.09
Physics
Fluid Dynamics
Scientific paper
Rotating magnetoconvection is a problem of central importance for understanding the origin and evolution of magnetic fields in stars and planets. In recent years, attention has turned increasingly away from the ``kinematic'' problem of generating magnetic fields in a prescribed flow, to the ``dynamic'' one, in which Lorentz forces are allowed to back-react on the flow as it proceeds to a preferred final state. This talk illustrates the complexities of steady-state magnetoconvection even in a highly idealized scenario. The rotating annulus model of Busse and Or (JFM, 1986) replaces the spherically stratified body of a star or planet; conducting side and end walls confine an imposed, azimuthal magnetic field, and the Taylor--Proudman theorem constrains the flow to planes orthogonal to the rotation axis. The virtue of this artificial system is that its nonlinear dynamics can be studied in detail through numerical simulations of the 2D MHD equations. Of special interest is the instability of the system to a mean (horizontally sheared) flow, as this is a proxy for differential rotation---an essential ingredient in dynamo models of the Sun, for instance. One goal of this talk is to show that in the weakly nonlinear regime, the shear instability can be explained by extending the models of Howard and Krishnamurti (JFM, 1986) and Lantz (ApJ, 1995) to include Coriolis effects. Bifurcations that appear as the vertical temperature gradient is increased are depicted using video visualizations of MHD simulation results.
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