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• W2133424077 abstract "HIRISE CAMERA N.T. Bridges 1 , E. Gorbaty 2 , R.A. Beyer 3 , S. Byrne 4 , B.J. Thomson 1 , J.J. Wray 5 and The HiRISE Team; 1 Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Dr., Pasadena, CA 91109 (nathan.bridges@jpl.nasa.gov); 2 Department of Geological and Environmental Sciences, Stanford University, Stanford, CA 94305-2115; 3 SETI Institute, Mountain View, CA 94043; 4 Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721; 5 Astronomy Dept., Cornell Univ., Ithaca, NY 14853 Introduction The High Resolution Imaging Science Experiment (HiRISE) on the Mars Reconnaissance Orbiter (MRO) provides unprecedented detail of geologic features on Mars [1]. One of HiRISE’s chief objectives is to provide a better understanding of aeolian (wind) features and processes. A summary paper of initial results was recently published [2]. Here we report in greater detail on the finding that much of the low thermal inertia mantle is organized into small “reticulate” ridges, which we interpret as bedforms. We show that the bedforms’ morphology and distribution are consistent with windblown (saltated) material, although the thermophysical properties indicating that these materials are dust-rich are difficult to reconcile with this hypothesis. Some yardangs have a texture similar to the reticulate forms, suggesting cementation over time. Background Viking IRTM observations showed that the summit regions of the Tharsis and Elysium volcanoes have low thermal inertias, consistent with a surface coated by fine (~2-40 !m), bright (albedo > 0.27) dust [3,4]. Later images from MOC showed a mantle that in many places partly or completely obscured details of the volcanic landforms, with wind tails and aeolian grooves common [5]. The general hypothesis for the formation of this mantle is that the high elevation volcanoes act as sinks for Martian dust that settles onto the surface following major dust storms [4]. Presumably the low pressures (<1 to ~2 mb) and therefore lack of sufficient shear stress to liberate significant dust off the surface allows it to accumulate over time. However, the formation of dark (albedo 0.2-0.3) collars within brighter annuli in the upper 10-20 km of the volcanoes, and the presence of downslope wind streaks at the base of the collars [6], indicates downslope winds that are probably induced by nighttime cooling [7]. Therefore, at least the upper surface in some regions is subject to aeolian transport. This may account for the wind tails and grooves described by [5]. The thermal inertia of high elevation materials does not have a unique signature [8], and there is evidence from the seasonal variability and diurnal differences in apparent inertia on the volcanoes of a heterogeneous surface [9], such that the interpretation of a pure dust surface may be overly simplistic. At HiRISE resolution, most mantled areas of the volcanoes are composed of networks of “reticulate” ridges down to scales of a few meters or less [2] (Fig. 12). Similar morphologies have also been seen in Valles Marineris, the equatorial lowlands, and other locations [10], although the distribution in these areas is not as pervasive." @default.
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• W2133424077 date "2008-03-01" @default.
• W2133424077 modified "2023-09-25" @default.
• W2133424077 title "LOW THERMAL INERTIA AND HIGH ELEVATION BEDFORMS AS SEEN BY THE HIRISE CAMERA" @default.
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