Vertical profiles of dust and ozone in the Martian atmosphere deduced from solar occultation measurements

Details Vertical profiles of dust and ozone in the Martian atmosphere deduced from solar occultation measurements Vertical profiles of dust and ozone in the Martian atmosphere deduced from solar occultation measurements

Feb 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991p%26ss...39..175b&link_type=abstract

(Colloquium on Phobos-Mars Mission, Paris, France, Oct. 23-27, 1989, Proceedings. A91-29558 11-91) Planetary and Space Science (

Astronomy and Astrophysics

Astronomy

19

Aerosols, Mars Atmosphere, Ozone, Spaceborne Astronomy, Vertical Distribution, Microprocessors, Mirrors, Onboard Equipment, Particle Telescopes, Phobos, Mars, Atmosphere, Dust, Ozone, Spacecraft Observations, Opacity, Haze, Optical Properties, Thickness, Water Ice, Clouds, Particles, Equipment, Size, Eddy Effects, Diffusion, Sedimentation, Ozone, Diagrams, Models, Procedure, Analysis, Altitude, Aerosols, Calculations, Parameters

Scientific paper

The vertical distribution of the ozone content and of the aerosols in the Martian atmosphere at the equinox and near the equator was studied with the aid of a biaxial pointing device, a microprocessor-controlled flat mirror of elliptical shape. An upper limit of 5 x 10 to the 7th mol/cu cm for ozone was obtained above an altitude of 30 km. For the aerosols, a semiquantitative distribution has been obtained between 10 and 50 km of altitude. The scale height is nearly equal to the atmospheric scale height in the 10-20 km region where mixing seems to predominate, and falls rapidly to a thickness of about 2 km at 30 km. In 10 percent of the occultations, a stratified haze has been detected between 40 and 50 km. The particle radius of cloud constituents is estimated and optical thickness per kilometer of these hazes at peak extinction are approximated. An eddy diffusion coefficient and a mixing ratio are estimated for clouds assumed to be at equilibrium.

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