|Impact melt, from nearby Egede A crater, formed channels as it flowed one kilometer down slope. Cracks in the melt probably formed as a result of cooling and inflation. Half-kilometer-wide field of view from LROC Narrow Angle Camera (NAC) frame M175204950LE, LRO orbit 10954, November 6, 2011; resolution 0.43 meters, in the original, an an incidence angle 63.49° from 29.54 kilometers [NASA/GSFC/Arizona State University].|
Impact melt creates spectacular morphologies on the Moon. Sometimes melt pools into large ponds, sometimes melt cascades down crater terraces, and sometimes melt forms channelized flows. The Egede A impact melt flows (as well as numerous other flows) are channelized with levees at their margins. Are there any analogues for channelized impact melt flows on Earth?
Yes! Levees occur naturally in terrestrial lava flows and develop as the edges of a lava flow cool and solidify. The lava flow can channelize with the levees help and make itself more thermally efficient. The levees allow the flow to travel farther from its source by slowing the cooling.
|LROC Wide Angle Camera context image of the LROC Featured Image released November 6, 2012 (located in the white box). Egede A is a 12.3 km crater at 51.57° N, 10.51 E, northeast of the Vallis Alpes. Monochrome (604 nm) mosaic stitched from subsequent observation opportunities in orbits 3132 and 3134, March 2, 2010; from LROC WAC observations M122130239C and M122143802C. Resolution average 59.9 meters per pixel from 42 kilometers[NASA/GSFC/Arizona State University]. [NASA/GSFC/Arizona State University].|
Explore more of Egede A crater in the full LROC NAC, HERE.
Winding Channel of Melt
Branched Impact Melts
Shadows in Egede A