Computer Science
Scientific paper
Jan 1981
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981icar...45...25j&link_type=abstract
Icarus, vol. 45, Jan. 1981, p. 25-38.
Computer Science
31
Infrared Imagery, Mars Surface, Radar Cross Sections, Surface Temperature, Thermal Mapping, Diurnal Variations, Dust, Permittivity, Remote Sensing, Soil Mapping, Viking Orbiter Spacecraft, Mars, Thermal Properties, Radar Observations, Comparisons, Scattering, Dielectric Constant, Size, Dust, Wavelengths, Density, Remote Sensing, Particles, Atmosphere, Longitude, Temperatures, Surface, Data, Models, Radioemissions
Scientific paper
Results of thermal infrared sensing and radar observations of the Martian surface are compared for the region centered on +22 deg latitude. Values of the apparent thermal inertia of the surface were derived from surface brightnesses observed by the Viking Orbiter Infrared Thermal Mapper, while radar cross sections were obtained in earth-based experiments at wavelengths of 3.8, 12.5 and 70 cm. A correlation between the thermal inertia and radar cross section values is observed which is strongest with the 70-cm radar data except between longitudes of 10 and 90 deg, where a slight anticorrelation is found. The mixing of small (much less than 70 cm) rocks into a surface of fine material can account for the data between 90 and 370 deg longitude, with as much as 50% of the surface covered by rock in Syrtis Major, Isidis Planitia and parts of Elysium Planitia, and little or no rock cover near Olympus Mons, Elysium Mons, and Amazonis Planitia. The remaining longitudes may be explained in terms of the effects of atmospheric dust on the surface temperature or the effects of local variations in large-scale roughness or scattering from rocks. Data from the 90 to 370 deg longitude region are consistent with the division of the Martian surface into two types of terrain, possibly related to the erosional or depositional nature of the regions.
Jakosky Bruce M.
Muhleman Duane O.
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