Computer Science
Scientific paper
Mar 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994cosre..31..540m&link_type=abstract
Cosmic Res., Vol. 31, No. 5, p. 540 - 561
Computer Science
Spectrophotometry: Mars Surface, Spectrophotometry: Mars Atmosphere
Scientific paper
The authors reanalyze data of the KRFM experiment in the Phobos project. They process all five complete photometric profiles available (each at eight wavelengths) and improve the calibration and the procedure for calculating the models. They estimate the optical depth of the permanent haze to be 0.1 < τ < 0.2. (i.e., it turns out to be considerably less than that predicted from Viking data). The imaginary part of the index of refraction of particles of the permanent haze varies smoothly from 0.015 at 315 nm to 0.005 at 550 nm. This corresponds to some basaltic material containing several per cent iron oxides. The clouds above large volcanos have an optical depth ≡0.1 and contain ≡5·10-6g·cm-2 of ice particles. They estimate all of the characteristics of particles of the permanent haze under the assumption that they have a γ size distribution with a model radius rm = 0.4 μm and α = γ = 1. A smoothness factor q = 0.5 is acceptable to first order to describe the photometric properties of the surface in the entire range 315 - 550 nm, although the authors do not rule out an increase in q with increasing wavelength. They estimate the mean radius of optically active soil particles to be 6 - 7 μm. The method of calculating photometric profiles of Mars is improved over all previously published versions, since it allows for the main features of the optical properties of the Martian atmosphere (the presence of true absorption and a strongly forward-extended scattering indicatrix) and surface (its nonorthotropic nature).
Ksanfomaliti L. V.
Moroz Vasiliy Ivanovich
Petrova Elena V.
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