Dust devil track density on Mars: a global map

Physics

Scientific paper

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0343 Planetary Atmospheres (5210, 5405, 5704), 3322 Land/Atmosphere Interactions (1218, 1631, 1843), 5415 Erosion And Weathering, 5470 Surface Materials And Properties, 6225 Mars

Scientific paper

Dust devil track (ddt) density was evaluated using The Generic Mapping Tool (Wessel and Smith), to produce isochronal and gridded color maps, based on 2000 (7 m/px or better) Mars Orbiter Camera (MOC) narrow angle (N/A) images selected using stratified random sampling. Ddt were counted in each image and the density (number of ddt/km2) was calculated. Ddt densities were gridded using 30 minute grid spacing to maximize detail while preserving general trends and then mapped according to season: Ls: 0 through 180° (northern spring and summer) and Ls: 180 through 360° (southern spring and summer). The peak ddt density occurs in the southern hemisphere (30 ddt/km2) centered at 30° W, 60°S. The northern hemisphere peak is 12 ddt/km2 and centered at 160°W, 60°N. Both hemispheres have a band of increased ddt density centered at 60°. The southern band correlates with albedo changes noted by Geissler (2005), suggesting that dust devils could be responsible for the observed albedo change. Both bands of elevated ddt density correlate with bands of increased thermal inertia; areas mapped as less dusty exposed bedrock. This relationship suggests that dust devils could contribute to exposing the bedrock by removing overlying dust. Both the norhtern and southern band of elevated ddt density correlate with moderate Thermal Emissions Spectrometer (TES) derived surface temperatures found in a narrow (~5° band) around 60° (N and S) and not the hottest surface temperatures (as might have been expected). If we use ddt density as a proxy for dust devil activity then dust devil activity is greatest when the temperature gradient is greatest, and not when surface temperature is highest.

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