Linear rille in Mare Tranquillitatis, the result of extensional stresses. What caused the offset in the rille on the east wall? LROC NAC M146858595LE, image width is 700 m [NASA/GSFC/Arizona State University].
A small amount of impact melt pooled and froze on the floor of this Copernican impact crater, and is 90 x 70 m in size. What process creates impact melt pools? LROC NAC M111972680LE, image width is 750 m [NASA/GSFC/Arizona State University].
These elongate flows formed during their race towards the floor of Reiner crater. Boulders have piled up at the base of the flows. Are the flows impact melt, or something else? Downslope is to the upper left. LROC NAC M135548391LE, image width is 500 m [NASA/GSFC/Arizona State University].
Many layers are present in the wall of Euler crater. The layers are interpreted to be individual lava flows that formed the lunar maria. LROC NAC M124763045LE, image width is 500 m [NASA/GSFC/Arizona State University].
An impact melt pool (lower right) within Das crater. Nearby boulders are the result of fractured impact melt, which have migrated downslope and formed talus (upper left). Uphill direction is to the top left. LROC NAC M136091866, image width is 600 m [NASA/GSFC/Arizona State University].