A geologic evaluation of thermal properties for the Elysium and Aeolis quadrangles of Mars

The results of an analysis of high-resolution thermal inertia data (obtained with the IR Thermal Mapper) for the Elysium and Aeolis quadrangles of Mars are presented. The results indicate that aeolian features, both with dark and light albedos relative to their surroundings, have thermal inertias higher than that of the surrounding terrains. On the other hand, terrains with distinctive surface relief do not have distinguishable thermal properties, even when these terrains can be spatially resolved from surrounding units. Thermal inertias for individual geologic units within the two quadrangles appear to be more strongly controlled by the location of the terrain in either the northern plains or the southern highlands than by properties intrinsic to the unit. The similarity of regional thermal properties observed at both high and low spatial resolutions indicates a regional homogeneity of much of the Martian surface at scales larger than 5 km.