Most aspects of the crater indicate that it was formed by impact. The dark material probably was penetrated at depth and ejected late in the explosive stage to accumulate in the vicinity of the rim. The light linear streaks and pointed markings are the rays from the fresh crater. In this picture the light material overlies dark regolith. The rim of the crater slopes steeply up from the mare surface, and the rim crest is sharp and even.
Boulders are abundant on and near the rim.
Concentric dunelike features occupy the inner part of the ejecta blanket and, with increasing distance from the crater, give way to irregular arcuate clusters of satellitic craters. A more subtle radial pattern in the ejecta can be seen where the Sun's rays shine across it, to the north and south of the crater. Most young lunar craters wider than about 40 km have flows on their rims that resemble lava flows or mud flows on Earth. Flows in the middle of the picture surged downhill off the high rim of the crater making lobes and tongues and leaving behind drained channels with levees. In the area to the right of the crater, enlarged in figure 104, are some thin lobate flows that apparently rode over small hills, as if these flows were propelled outward from the crater with sufficient velocity to climb the hills.