Effects of dust on radiation transfer in the Martian atmosphere. III - Numerical experiments of radiative-convective equilibrium of the Martian atmosphere including the radiative effects due to dust

Details Effects of dust on radiation transfer in the Martian atmosphere. III - Numerical experiments of radiative-convective equilibrium of the Martian atmosphere including the radiative effects due to dust Effects of dust on radiation transfer in the Martian atmosphere. III - Numerical experiments of radiative-convective equilibrium of the Martian atmosphere including the radiative effects due to dust

Feb 1976

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976mesjj..54...52m&link_type=abstract

Meteorological Society of Japan, Journal, vol. 54, Feb. 1976, p. 52-58.

Mathematics

Logic

Atmospheric Heat Budget, Atmospheric Temperature, Convective Heat Transfer, Mars Atmosphere, Radiant Cooling, Radiative Heat Transfer, Atmospheric Heating, Dust Storms, Infrared Radiation, Particle Size Distribution, Solar Heating, Temperature Inversions, Temperature Profiles

Scientific paper

The radiative-convective equilibrium of the Martian atmosphere is studied for a range of solar zenith angles. Heating due to absorption of solar radiation by dust; infrared radiative cooling by dust; and cooling by CO2 (15-micron band) are taken into consideration. Numerical calculations indicate that the dusty Martian atmosphere has a stable thermal structure and that the temperature is higher than in the dust-free case. The dusty atmosphere is heated directly by absorption of solar radiation, rather than by heat trasnport by convection from the lower layers. In the case of long optical path lengths of solar radiation, a thick inversion layer appears at the upper levels even during daytime.

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