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Absorption and scattering properties of the Martian dust in the solar wavelengths
Maureen E. Ockert-Bell,
James F. Bell III,
James B. Pollack,
Christopher P. McKay,
François Forget,
Maureen E. Ockert-Bell
Search for more papers by this authorJames F. Bell III
Search for more papers by this authorJames B. Pollack
Search for more papers by this authorChristopher P. McKay
Search for more papers by this authorFrançois Forget
Search for more papers by this authorMaureen E. Ockert-Bell,
James F. Bell III,
James B. Pollack,
Christopher P. McKay,
François Forget,
Maureen E. Ockert-Bell
Search for more papers by this authorJames F. Bell III
Search for more papers by this authorJames B. Pollack
Search for more papers by this authorChristopher P. McKay
Search for more papers by this authorFrançois Forget
Search for more papers by this authorAbstract
A new wavelength-dependent model of the single-scattering properties of the Martian dust is presented. The model encompasses the solar wavelengths (0.3 to 4.3 μm at 0.02 μm resolution) and does not assume a particular mineralogical composition of the particles. We use the particle size distribution, shape, and single-scattering properties at Viking Lander wavelengths presented by Pollack et al. [1995]. We expand the wavelength range of the aerosol model by assuming that the atmospheric dust complex index of refraction is the same as that of dust particles in the bright surface geologic units. The new wavelength-dependent model is compared to observations taken by the Viking Orbiter Infrared Thermal Mapper solar channel instrument during two dust storms. The model accurately matches afternoon observations and some morning observations. Some of the early morning observations are much brighter than the model results. The increased reflectance can be ascribed to the formation of a water ice shell around the dust particles, thus creating the water ice clouds which Colburn et al. [1989], among others, have predicted.
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