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Impact spallation is a fundamental process responsible for formation of ejecta boulders from impact craters. Although theoretical spallation models were developed about three decades ago, only limited geological observations have been made so far to test these models. The 3.8km Censorinus crater on the Moon provides an excellent opportunity for studying the impact spallation processes associated with...
The lunar surface is characterized by asymmetric distribution of its volcanic deposits. The nearside contains about 90% of the mare basalts, while there are a few on the farside with some are in the South Pole Aitken (SPA) basin, which is the largest and oldest impact basin on the Moon. Although the mare volcanism on the nearside of the Moon has been very well characterized, our understanding of the...
Analysis of the Chandrayaan-1 Terrain Mapping Camera image of a 20km×27km area in the Mare Imbrium region revealed a cluster of thousands of fresh and buried impact craters in the size range of 20–1300m. A majority of the large fresh craters with diameter ranging from 160 to 1270m exhibit near-circular mounds (30–335m diameter and 10–40m height) in the crater floor, and their size depends on the host...
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