Mars - Far-infrared spectra and thermal-emission models

Details Mars - Far-infrared spectra and thermal-emission models Mars - Far-infrared spectra and thermal-emission models

Nov 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981icar...48..230s&link_type=abstract

Icarus, vol. 48, Nov. 1981, p. 230-245.

Computer Science

29

Atmospheric Models, Far Infrared Radiation, Infrared Spectra, Mars Atmosphere, Planetary Radiation, Thermal Emission, Mars Surface, Particle Size Distribution, Silicates, Surface Temperature, Mars, Infrared, Spectra, Emissions, Models, Thermal Effects, Brightness, Kao Aircraft, Aircraft Observations, Surface, Comparisons, Parameters, Emissivity, Wavelengths, Particles, Temperature, Dust, Composition, Size, Atmosphere, Optical Properties, Depth, Albedo, Polar Regions, Ice Caps

Scientific paper

Spectra of Mars from 100 to 360 kaysers were obtained during three different observation periods from NASA's Kuiper Airborne Observatory. Also, a new thermal model was constructed for the surface of Mars, and synthetic spectra were computed from the models to compare with the observations. The models include the effects of a dusty atmosphere which absorbs, scatters, and reradiates energy. The synthetic spectra show significant effects on disk-averaged brightness temperatures, as well as absorption features due to silicate dust. The spectra of Mars, which are ratios of Mars to the moon, do not fit the synthetic spectra unless the surface emissivities of Mars and the moon have different dependencies on wavelength. A possible explanation for this behavior is a difference in soil particle-size distributions between Mars and the moon, with Mars being depleted in large particles compared to the moon. Small particles are consistent with clay minerals which have been suggested elsewhere as constituents of the Martian surface.

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