Computer Science – Numerical Analysis
Scientific paper
Feb 1976
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976jats...33..321z&link_type=abstract
Journal of the Atmospheric Sciences, vol. 33, Feb. 1976, p. 321-337. NASA-supported research.
Computer Science
Numerical Analysis
34
Atmospheric Tides, Diurnal Variations, Mars Atmosphere, Mars Surface, Topography, Atmospheric Boundary Layer, Atmospheric Turbulence, Clear Air Turbulence, Dust Storms, Elevation, Numerical Analysis, Velocity Distribution, Wind Profiles
Scientific paper
Classical atmospheric tidal theory is extended to include the effects of large-amplitude planetary-scale variations of the terrain height. Utilizing simple models of the thermotidal forcing, the resulting technique is used to compute the diurnal tide in both the dust-free and the dust-laden Martian atmosphere. The main effect of the Martian variable terrain is to drive topographic tidal modes which can propagate vertically and to excite the possibly resonant diurnal Kelvin mode. The resulting surface wind can exceed 20 m/sec and may determine the preferred location for the initiation of global dust storms. In the middle Martian atmosphere (30-80 km) static and shear instabilities embedded within the tidal fields will generate extensive, though variable, regions of turbulence. Vertical mixing by this turbulence and transport by the tide itself may help to stabilize the middle Martian atmosphere against photolysis.
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