Regional dust deposits on Mars - Physical properties, age, and history

Mathematics – Logic

Scientific paper

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Dust Storms, Mars Environment, Mars Surface, Planetary Evolution, Planetary Geology, Albedo, Deposition, Mars Atmosphere, Planetary Mapping, Planetary Orbits, Regolith, Thermal Mapping, Viking Spacecraft, Wind Erosion, Mars, Dust, Deposits, Physical Properties, Age, History, Deposition, Storms, Remote Sensing, Regolith, Tharsis Region, Radar Methods, Wind, Arabia Region, Elysium Region, Texture, Brightness, Particles, Models, Thickness, Velocity, Transport, Parameters, Distribution, Formation, Erosion, Surf

Scientific paper

This paper presents a description of the use of Viking infrared thermal mapper (IRTM), earth-based radar, and visual observations for the study of the existence of regional dust deposits. It is pointed out that these observations provide estimates of particle size, rock abundance, surface texture, thermal emissivity, and albedo. These estimates can be used to characterize surface deposits and to determine the degree of surface mantling. Attention is given to the regolith properties, atmospheric dust properties, and a model for formation of low-inertia regions. It is found that global dust storms deposit currently approximately 25 microns of material per year in the equatorial region. Over geologic time this value may vary from 0 to 250 microns due to variations in atmospheric conditions produced by orbital variations.

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