Polar symmetric flow of a viscous compressible atmosphere - an application to Mars

Details Polar symmetric flow of a viscous compressible atmosphere - an application to Mars Polar symmetric flow of a viscous compressible atmosphere - an application to Mars

Jan 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975jats...32...60p&link_type=abstract

Journal of the Atmospheric Sciences, vol. 32, Jan. 1975, p. 60-72.

Computer Science

1

Atmospheric Circulation, Atmospheric Temperature, Compressible Flow, Eddy Viscosity, Mars Atmosphere, Viscous Flow, Atmospheric Boundary Layer, Atmospheric Models, Boundary Conditions, Boundary Layer Transition, Dust Storms, Geostrophic Wind, Mariner 9 Space Probe, Meridional Flow, Pressure Gradients, Temperature Distribution, Velocity Distribution, Vorticity Equations

Scientific paper

The atmosphere is assumed to be driven by a polar symmetric temperature field. The surface pressure gradient exhibits a latitudinal dependence opposite that of the depth-averaged temperature. The magnitude of the gradient is dependent upon the depth of the boundary layer, which depends upon the eddy viscosity, the boundary conditions imposed at the surface, and upon the temperature lapse rate. Using a temperature model for Mars based on Mariner 9 infrared spectral data with a 30% increase in the depth-averaged temperature from the winter pole to the subsolar point, the increase in surface pressure from the subsolar point to the winter pole was calculated as a function of eddy viscosity with no-slip conditions imposed at the surface. The meridional cellular flow rate is correlated with the eddy viscosity, causing a complete overturning of the atmosphere in tens of days for an eddy viscosity of .1 billion sq cm/sec and in hundreds of days for 1 million sq cm/sec. The implication of this overturning in the dust storm observed during the early part of the Mariner 9 mission is discussed briefly.

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