Theoretical interpretation of photometric properties of the Martian surface and atmosphere

Astronomy and Astrophysics – Astronomy

Scientific paper

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Astronomical Photometry, Dust Storms, Limb Darkening, Mars Atmosphere, Mars Surface, Radiative Transfer, Albedo, Astronomical Photography, Mariner 9 Space Probe, Optical Thickness, Surface Roughness, Ubv Spectra, Mars, Photometry, Physical Properties, Surface, Atmosphere, Isophotes, Theoretical Studies, Ultraviolet, Mathematical Models, Mariner 9, Data, Earth-Based Observations, Radiative Transfer, Dust Storms, Particles, Albedo, Scattering, Optical Properties, Thickness, Wavelengths, Soils, Asymmetry, Comp

Scientific paper

Earth-based UBV photometry, photographs from the Lowell Observatory, and Mariner 9 data are combined with a new radiative transfer theory to derive physical parameters for the Martian surface and atmosphere, both before and during the 1971 dust storm. Storm dust particles had a single scattering albedo of 0.84 plus or minus 0.02 and an asymmetry factor of 0.35 plus or minus 0.10 in green (V) light. The geometric albedo of Mars was 0.15 and the phase integral 1.83, yielding 0.27 for the Bond albedo. The mean optical thickness of the 'clear' atmosphere averaged over the whole planet was 0.15 plus or minus 0.05 and was not dependent on wavelength. Geometric albedos for the surface are 0.25 (light areas) and 0.17 (dark areas) in V, 0.095 in B, and 0.060 in U. The soil particles are moderately backward scattering with an asymmetry factor of minus 0.20, and therefore rather opaque. The mean surface roughness is 0.57, representing the depth/radius ratio of an average hole, and being only one-half as large as values typical for the moon and asteroids.

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