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Rock Avalanche in Robinson Crater

Published by Matt on Wed Nov 24, 2010 10:52 am via: NASA
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An impact crater changes its shape with time by various degradation processes, such as wall slumping, infilling with ejecta deposits from nearby impacts, and volcanic activities. Rock avalanches as shown in today’s featured image also contribute to modifying crater shape little by little.

Northern slope inside Robinson crater. LROC NAC M114259768R, 0.52 m/pixel, image width is 620 m, sun light is from right side. Slope direction is from top to the bottom of the image Credit: NASA/GSFC/Arizona State University.

Northern slope inside Robinson crater. LROC NAC M114259768R, 0.52 m/pixel, image width is 620 m, sun light is from right side. Slope direction is from top to the bottom of the image Credit: NASA/GSFC/Arizona State University.

Multiple tongue shaped flow fronts in this image evoke liquid (Newtonian) flow features, especially mudflows. Similar features have been found on Mars, and are interpreted to represent recent mudflows. Water is not stable on the Moon’s surface (except perhaps as ice in permanently shadowed craters), so these flows are dry (granular) rock slides. Perhaps some of the flow features on Mars thought to indicate wet mudflows are really dry granular flows?

Context map of Robinson crater. Image center is 314.0°E, 59.1°N. LROC WAC 100 m/px monochrome global mosaic overlayed by WAC color DTM 500 m/px. The blue box corresponds to the footprint of today's featured NAC image. Credit: NASA/GSFC/Arizona State University

Context map of Robinson crater. Image center is 314.0°E, 59.1°N. LROC WAC 100 m/px monochrome global mosaic overlayed by WAC color DTM 500 m/px. The blue box corresponds to the footprint of today's featured NAC image. Credit: NASA/GSFC/Arizona State University

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