Thermal inertia mapping of Mars from 60 deg S to 60 deg N

Details Thermal inertia mapping of Mars from 60 deg S to 60 deg N Thermal inertia mapping of Mars from 60 deg S to 60 deg N

Feb 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981icar...45..415p&link_type=abstract

Icarus, vol. 45, Feb. 1981, p. 415-426.

Mathematics

Logic

193

Brightness Temperature, Inertia, Mars Surface, Planetary Mapping, Remote Sensing, Thermal Mapping, Albedo, Cosmic Dust, Planetary Temperature, Specific Heat, Surface Properties, Temperature Measurement, Thermal Conductivity, Viking Orbiter Spacecraft, Mars, Mapping, Thermal Properties, Brightness Temperatures, Irtm, Maps, Latitude, Viking Infrared Thermal Mapper, Dust Storms, Albedo, Imagery, Distribution, Dust, Deposition, Temperatures, Radio Waves, Surface, Infrared, Wavelengths, Calibrations, Data, Techn

Scientific paper

The considered region comprises 81% of the surface of Mars. Thermal inertia I is a composite surface property, which is equal to the square root of the product of three factors, including the thermal conductivity, the density, and the specific heat. I is the sole thermal parameter which governs the temperature variation of a periodically heated homogeneous surface, and, as such, is the prime intermediary between remote temperature observations and their geologic interpretation. The values for the thermal inertia found imply particulate surface materials. The variation in Martian surface thermal conductivity is about two orders of magnitude. Three large regions of low-inertia material are defined. Low-inertia material always possesses high albedo. There is a general tendency for higher-thermal-inertia surfaces to be darker but exceptions occur which may be related to a thin mantling of light dust or bonding of light material.

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