Quasi-axisymmetric circulation and superrotation in planetary atmospheres

Details Quasi-axisymmetric circulation and superrotation in planetary atmospheres Quasi-axisymmetric circulation and superrotation in planetary atmospheres

May 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983a%26a...121..124m&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 121, no. 1, May 1983, p. 124-136.

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Anisotropic Fluids, Atmospheric Circulation, Axisymmetric Flow, Planetary Atmospheres, Superrotation, Viscous Fluids, Atmospheric Heat Budget, Atmospheric Models, Atmospheric Temperature, Computational Fluid Dynamics, Jupiter Atmosphere, Three Dimensional Models, Turbulent Diffusion, Two Dimensional Models, Venus Atmosphere, Venus Clouds, Planets, Atmosphere, Circulation, Rotation, Models, Spectra, Fluids, Diffusion, Flow, Solar Radiation, Absorption, Energy, Pressure, Thermal Effects, Altitude, Hydrodynami

Scientific paper

Atmospheric superrotation is ubiquitous in the solar system, and numerous theoretical models have been proposed to describe the effect. However, no model is fully accepted. Problems are primarily related to an understanding of the angular momentum and the energy budgets. In connection with the present investigation, attention is given to hybrid models, where three-dimensional models may describe eddy processes and two-dimensional symmetric models may describe the global scale circulation in the framework of a viscous medium. It is believed that the concept of an axisymmetric circulation is still useful. It is the main purpose of the current investigation to explore some of the properties of the circulation in planetary atmospheres. It is assumed that the eddy transports are downgradient or diffusive in nature. Energy and momentum are perceived to cascade from the global scale circulation driven by the sun to the smaller scale eddies which in turn determine the diffusive properties. A numerical model of the Venusian circulation is presented, and results are discussed for different conditions of static stability.

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