Dust in the Martian Atmosphere: Polarimetric Sensing

Details Dust in the Martian Atmosphere: Polarimetric Sensing Dust in the Martian Atmosphere: Polarimetric Sensing

May 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993a%26a...272..671e&link_type=abstract

Astronomy and Astrophysics, vol. 272, 671-686. Article.

Astronomy and Astrophysics

Astrophysics

14

Martian Atmosphere, Dust Storms, Polarimetry, Mars, Atmosphere, Dust, Polarimetry, Dust Storms, Polarization, Haze, Earth-Based Observations, Anomalies, Analysis, Solar Effects, Heating, Particles, Grain Size, Seasonal Variations, Evolution, Reflectance, Density, Optical Properties, Depth, Timescale, Lifetime

Scientific paper

Several thousands of determinations of the degree of linear polarization have been recorded over the disk of Planet Mars, at Tokyo Observatory station, from 1977 to 1991.
In addition to the polarization produced by reflectance over the Martian soil surface, there is some perturbations by local veils of crystal or by dust storms which have been already analyzed. But a new type of unusual event has been discovered, displaying temporary anomalies in the degree of polarization. Their analysis characterizes faint and transparent veils, localized over specific areas, and at certain times of the Martian year corresponding to the maximum solar heating. The scattering theory of Mie indicates solid, absorbing sub-micron size grains, reminiscent of small dust particles raised from the soil surface.
Dust is observed in the Martian atmosphere at three levels: (1) a permanent faint haze made of very small dust particles. (2) Temporary local transparent veils made of submicron size grains, preferentially during seasons and latitudes of maximum solar heating. (3) Occasionally, an evolution of these veils to produce extensive, dense, dust storms made of micron size grains, which may spread all over the planet for weeks.

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