Degradation of large, period II lunar craters

Nighttime thermal maps of large, young lunar craters show an evolutionary sequence in the gross morphology of thermal patterns associated with the craters. The nature of the sequence is consistent with crater degradation models which predict a filling of large craters with material from the walls. Detailed comparison of a nighttime thermal map of Copernicus with a geologic map demonstrates that a smooth floor unit characterized as impact melt is more likely wall debris. Nighttime thermal maps will be particularly useful for quantifying crater modification which has occurred in the relatively quiescent post-basin period of lunar history.