Parameterized rotating convection for core and planetary atmosphere dynamics

Details Parameterized rotating convection for core and planetary atmosphere dynamics Parameterized rotating convection for core and planetary atmosphere dynamics

Apr 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991georl..18..685z&link_type=abstract

Geophysical Research Letters (ISSN 0094-8276), vol. 18, April 1991, p. 685-688. Leverhulme Trust-supported research.

Physics

2

Digital Simulation, Planetary Atmospheres, Planetary Cores, Prandtl Number, Rotating Spheres, Buoyancy, Geomagnetism, Rayleigh Number, Planets, Atmosphere, Dynamics, Convection, Core, Numerical Methods, Simulations, Stability, Diagrams, Flow, Temperature, Calculations, Rotation, Fluids, Thermal Effects, Viscosity, Hydrodynamics, Jets, Symmetry, Gas Planets, Outer Planets

Scientific paper

New types of convective instability and associated nonlinear phenomena in rapidly rotating spherical systems have been discovered through numerical simulations. The Prandtl number, defined as the ratio of the viscous and thermal diffusivities of a fluid, Pr = nu/kappa, plays a crucial role in determining the fundamental features of both the instabilities and the corresponding nonlinear convection. The results shed new light on regimes of convection in the earth's core and the atmospheres of the major planets.

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