Complex refractive index of Martian dust - Wavelength dependence and composition

Details Complex refractive index of Martian dust - Wavelength dependence and composition Complex refractive index of Martian dust - Wavelength dependence and composition

Jan 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977icar...30...63p&link_type=abstract

Icarus, vol. 30, Jan. 1977, p. 63-74.

Computer Science

18

Atmospheric Refraction, Dust Storms, Mars Atmosphere, Particle Size Distribution, Ultraviolet Spectra, Absorption Spectra, Albedo, Mariner 9 Space Probe, Mars Surface, Mie Scattering, Optical Density, Satellite-Borne Instruments, Spectrum Analysis, Titanium Oxides, Ultraviolet Spectrometers

Scientific paper

The size distribution and complex refractive index of Martian dust-cloud particles observed in 1971 with the Mariner 9 UV spectrometer are determined by matching the observed single-scattering albedo and phase function with Mie-scattering calculations for size distributions of spheres. Values of phase function times single-scattering albedo are presented for 12 wavelength intervals in the range from 190 to 350 nm, and best-fit values are obtained for the absorption index. It is found that the absorption index of the dust particles increases with decreasing wavelength from 350 to about 210 nm and then drops off shortward of 210 nm, with a structural shoulder occurring in the absorption spectrum between 240 and 250 nm. A search for a candidate material that can explain the strong UV absorption yields TiO2, whose anatase polymorph has an absorption spectrum matching that of the Martian dust. The TiO2 content of the dust particles is estimated to be a few percent or less.

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