Analysis of Martian atmospheric and surface optical properties between 4.4 and 5.1 microns

Details Analysis of Martian atmospheric and surface optical properties between 4.4 and 5.1 microns Analysis of Martian atmospheric and surface optical properties between 4.4 and 5.1 microns

Sep 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992msat.work...39c&link_type=abstract

In Lunar and Planetary Inst., Workshop on the Martian Surface and Atmosphere Through Time p 39-40 (SEE N92-28988 19-91)

Other

Mars Atmosphere, Mars Surface, Mie Scattering, Optical Properties, Surface Properties, Albedo, Algorithms, Basalt, Carbon Dioxide, Dust, Infrared Telescopes, Mars (Planet), Spectrometers, Water

Scientific paper

Spectra of several regions of Mars were taken by Blaney and McCord in Aug. of 1988 with the Cooled Grating Array Spectrometer (CGAS) at the NASA Infrared Telescope Facility (IRTF). The resulting spectra show several distinct absorption features at wavelengths between 4.4 and 5.1 microns. Many of these features can be attributed to gases in the Martian atmosphere, but others are more difficult to identify. To analyze these spectra more completely, we used a line-by-line multiple scattering model that was developed for studies of Venus night-side emission. This model includes all atmospheric and surface radiative processes that are known to be important on Mars, including absorption, emission, and multiple scattering by CO2, H2O, CO, and airborne dust, and a spectrally-dependent surface albedo. A Mie-scattering algorithm was used to derive dust optical properties from the optical constants of palagonic and basalt. Results from our preliminary efforts to simulate the spectra taken near Tharsis and Solis Planum are shown.

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