Abstract
WITH remarkably few exceptions, the inner floors of typical rimmed lunar craters lie below the external datum (which is the base of the crater outer rim) whereas floors of terrestrial calderas are situated well above the base of the host volcano. Gilbert1, the first to describe this fundamental difference in the surface geometry of the two landforms, referred specifically to “normal” or “main sequence” lunar craters such as Copernicus or Alphonsus, with which lunar observers were most familiar. His generalization does not necessarily extend to lunar dome and cone summit craters, various types of rimless depressions and chain craters, or to normal craters which have been deeply and catastrophically flooded or buried by post-formational geologic materials. This distinction is continued in this communication.
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