New views of Mars eolian activity, materials, and surface properties : Three vignettes from the Mars Global Surveyor Mars Orbiter Camera

By K. Edgett, Michael C. Malin. 2000

163 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Atmospheric Science, Earth-Surface Processes

View Paper: https://www.semanticscholar.org/paper/84bcadf6a1c2b441a466f886afb89c56343add87

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Citations in the corpus

Context Camera Investigation on board the Mars Reconnaissance Orbiter (2007, background): “Comparisons between dune positions in Mariner 9 and Viking orbiter images with MGS MOC images (and MOC images with earlier MOC images) of dunes and large ripples have not yet revealed any evidence that the bedforms have moved during the past Martian decade [Edgett and Malin, 2000; Zimbelman, 2000; E”
High-resolution thermal inertia derived from the Thermal Emission Imaging System (THEMIS): Thermal model and applications (2006, background): “In the absence of direct observations of dune migration in visible images [Zimbelman, 2000; Edgett and Malin, 2000; Malin and Edgett, 2001], it is difficult to determine with confidence the current activity of bed forms.”
Modelling Desert Dune Fields Based on Discrete Dynamics (2002, background): “Furthermore, dune fields are also found on Mars (Greeley and Iversen, 1985 and Edgett and Malin, 2000) and Venus (Greeley et al., 1992).”
An overview of the 1985-2006 Mars Orbiter Camera science investigation (2010, background): “No examples of eolian crossbeds were unambiguously identified in MOC images, but at least one example of a lithified eolian dune field was found (Edgett and Malin 2000, Malin and Edgett 2001), a second site in Melas Chasma near 11.2°S, 75.2°W, might also consist of lithified dunes, and a very large…”
Mars Global Surveyor Mars Orbiter Camera: Interplanetary cruise through primary mission (2001, background): “MOC NA images show, as noted above, that some low albedo regions—particularly in Terra Meridiani and Sinus Sabaeus—are covered by mantles of material probably deposited from suspension and do not exhibit much evidence of windblown sand [Edgett and Malin, 2000a].”
Active dust devils in Gusev crater, Mars: Observations from the Mars Exploration Rover Spirit (2006, background): “surface. More recently, Edgett and Malin [2000a, 2000b] found numerous dust devils, some as high as 6 km, from analyses of Mars Orbiter Camera (MOC) images.”
Martian dust devils: Laboratory simulations of particle threshold (2003, background): “…al., 1999, 2002], Mars Global Surveyor (MGS), and Mars Odyssey missions confirm the presence of abundant aeolian features, including duneforms seen in Mars Orbiter Camera (MOC) high-resolution images [Malin et al., 1998; Malin and Edgett, 1999, 2001; Edgett and Malin, 2000a; Cantor et al., 2001].”
Modeling the Martian dust cycle, 1. Representations of dust transport processes (2002, methodology): “No global maps of dust devil occurrence are currently available, but recent MOC images [Edgett and Malin, 2000b] have shown them to occur in nearly every environment where imaging has allowed a search for the narrow, dark streaks, with rapid changes in direction, which signify their passage.”
Mars Reconnaissance Orbiter's High Resolution Imaging Science Experiment (HiRISE) (2007, methodology): “Dust Devils and Wind Streaks [126] Dust devils occur when the surface is heated appreciably such that convective heat transfer to the atmosphere takes place, and have been observed from orbit [Thomas and Gierasch, 1985; Edgett and Malin, 2000].”
The case for rainfall on a warm, wet early Mars (2002, background): “MOC images show that eolian deposition and scour in craters occurs in spatial patches considerably smaller than the size of large basin floors [Edgett and Malin, 2000].”