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We analyze thermal emission spectra using the 2001 Mars Odyssey ThermalEmission Imaging System (THEMIS) and the Mars Global Surveyor (MGS) ThermalEmission Spectrometer (TES) to characterize grain size and mineralogicalcomposition of dunes at Hargraves crater, Mars. Thermal inertia and bulkcomposition of the dunes were compared to inferred provenances from the thermalinfrared response of surface constituent materials. We use a Markov Chain MonteCarlo (MCMC) technique to estimate the bulk amount of mineralogy contributed byeach inferred provenance to the dune field composition. An average thermalinertia value of 238+/-17 Jm-2K-1s-0.5 was found for the dunes corresponding toa surface composed of an average effective grain size of ~391+/-172 um. Thiseffective particle size suggests the presence of mostly medium sand-sizedmaterials mixed with fine and coarse grain sands. The dunes are likelycomprised of a weakly indurated surface mixed with unconsolidated materials.Compositional analysis specifies that the dunes are comprised of a mixture offeldspar, olivine, pyroxene, and relatively low bulk-silica content. Dunematerials were likely derived from physical weathering, especially eolianerosion, predominantly from the crater ejecta unit at the crater, mixed with asmall amount from the crater floor and crater rim and wall lithologies -indicating the dune materials were likely sourced locally.

Thermophysical and Compositional Analyses of Dunes at Hargraves Crater, Mars