A comparative study of daytime thermally induced upslope flow on Mars and earth

Details A comparative study of daytime thermally induced upslope flow on Mars and earth A comparative study of daytime thermally induced upslope flow on Mars and earth

Mar 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990jats...47..612y&link_type=abstract

Journal of the Atmospheric Sciences (ISSN 0022-4928), vol. 47, March 1, 1990, p. 612-628.

Computer Science

18

Earth Atmosphere, Earth Surface, Flow Characteristics, Heat Flux, Mars Atmosphere, Mars Surface, Atmospheric Boundary Layer, Atmospheric Models, Atmospheric Temperature, Daytime, Geostrophic Wind, Mesoscale Phenomena, Planets, Mars, Earth, Thermal Effects, Flow, Comparisons, Analysis, Numerical Methods, Heating, Wind, Velocity, Depth, Temperature, Layers, Meteorology, Circulation, Calculations, Atmosphere, Parameters, Models, Simulations, Solar Radiation, Flux, Absorption, Surface, Turbulence, Friction, Bou

Scientific paper

Several characteristics of thermally induced mesoscale upslope flow on Mars and its comparison with that on earth were investigated using both analytical and numerical model approaches. The conclusions obtained from the analytical and the numerical evaluations of Mars are generally in agreement. The intensity of the Martian summer daytime upslope flow, with a moderate slope, reaches nearly 10 m/s and its depth is about 5 km. The longwave radiation flux divergence heating, within the lower boundary layer of Mars, has a nonnegligible contribution to the intensity of the upslope flows. On Mars, the values of upslope wind speed are, typically, about 2.5 times larger than on earth under similar conditions.

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