Origin and relative age of lunar and Mercurian intercrater plains

Abstract Differences in the diameter/density distribution of craters in the size range 7–100 km between heavily cratered areas and areas of intercrater plains indicate the deposition of both lunar and Mercurian intercrater plains has preferentially obliterated craters ⪝30 km diameter. This obliteration has altered the original lunar population distribution function from about a −1.3 slope to about a −0.7 slope. At least a significant portion of both the lunar and Mercurian intercrater plains appear to be volcanic deposits emplaced during the later stages of heavy bombardment on each body rather than basin ejecta or an ancient primordial surface. The very widespread distribution of intercrater plains on Mercury compared to the moon may be related to Mercury's core formation which would have resulted in a large radius increase leading to widespread extensional fracturing to provide egress for the eruption of volcanic deposits on a global scale. This was followed by a radius decrease due to contraction of the lithosphere to produce thrust faulting represented by Mercury's lobate scarps.