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Mie scattering and the Martian atmosphere

Published online by Cambridge University Press:  14 August 2015

Walter G. Egan  and
Kenneth M. Foreman
Walter G. Egan
Affiliation:
Research Dept., Grumman Aerospace Corporation, Bethpage, N.Y., U.S.A.
Kenneth M. Foreman
Affiliation:
Research Dept., Grumman Aerospace Corporation, Bethpage, N.Y., U.S.A.

Abstract

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It has been suggested that the discrepancy between radio occultation determinations of the Martian atmospheric surface pressure (3.8 to 7 mb) and those deduced from optical polarization measurements and a simple Rayleigh atmosphere model (about 10 mb) are the results of sub-micron sized aerosols in the Martian atmosphere. Based on observed viewing angle dependence of the polarization of the Martian disk in the visual range, a Mie scattering analysis has been made utilizing the measured complex index of refraction of limonite and bulk solid CO2. The results of this study indicate that limonite aerosols alone are unsatisfactory to explain the viewing angle observations, whereas solid CO2 (and H2O ice) aerosol spheres, having a dominant particle radius range between 0.28 and 0.35 μ, could bring planetary and laboratory observations into compatibility. It is suggested, further, that solid CO2 aerosols could explain limb brightening in the blue spectral range. Various distributions of solid CO2 and H2O Mie particles with radii up to 0.35 μ show an opposition effect. However, the role of these aerosols in explaining the Mars opposition observations is very dependent on the optical properties of the underlying Mars surface material.

Type
Part II: Mars
Information
Symposium - International Astronomical Union , Volume 40: Planetary Atmospheres , 1971 , pp. 156 - 165
Copyright
Copyright © Reidel 1971 

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