Martian particle size based on thermal inertia corrected for elevation-dependent atmospheric properties

Details Martian particle size based on thermal inertia corrected for elevation-dependent atmospheric properties Martian particle size based on thermal inertia corrected for elevation-dependent atmospheric properties

Mar 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993lpi....24..189b&link_type=abstract

In Lunar and Planetary Inst., Twenty-fourth Lunar and Planetary Science Conference. Part 1: A-F p 189-190 (SEE N94-12015 01-91)

Physics

Atmospheric Pressure, Inertia, Mars Surface, Particle Size Distribution, Thermal Conductivity, Thermal Mapping, Atmospheric Effects, Atmospheric Radiation, Elevation, Thermal Emission, Topography

Scientific paper

Thermal inertia is commonly used to derive physical properties of the Martian surface. If the surface is composed of loosely consolidated grains, then the thermal conductivity derived from the inertia can theoretically be used to compute the particle size. However, one persistent difficulty associated with the interpretation of thermal inertia and the derivation of particle size from it has been the degree to which atmospheric properties affect both the radiation balance at the surface and the gas conductivity. These factors vary with atmospheric pressure so that derived thermal inertias and particle sizes are a function of elevation. By utilizing currently available thermal models and laboratory information, a fine component thermal inertia map was convolved with digital topography to produce particle size maps of the Martian surface corrected for these elevation-dependent effects. Such an approach is especially applicable for the highest elevations on Mars, where atmospheric back radiation and gas conductivity are low.

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