Paul Spudis

TL;DR: In the course of 71 days in lunar orbit, from 19 February to 3 May 1994, the Clementine spacecraft acquired just under two million digital images of the moon at visible and infrared wavelengths, enabling the global mapping of the rock types of the lunar crust and the first detailed investigation of the geology of the Lunar polar regions and the lunar far side.

TL;DR: In this paper, a comparison between LROC NAC block populations, Mini-RF data, and Diviner-derived rock abundances confirm that blocky lava flows comprise the domes of the Marius Hills.

TL;DR: The Mini-SAR as mentioned in this paper is a single frequency (S-band; 13-cm wavelength) Synthetic Aperture Radar (SAR) in a lightweight (~9 kg) package, which utilizes a unique hybrid polarization architecture, which allows determination of the Stokes parameters of the reflected signal, intended to distinguish volume scattering (caused by the presence of ice) from other scattering mechanisms (e.g. sub-wavelength scale surface roughness).

TL;DR: In this article, a global topographic map of the Moon surface has been produced by combining these polar terrain models with the current Clementine laser altimeter data, including three previously unrecognized pre-Nectarian impact basins.

TL;DR: For example, the authors in this article show that the timing, extent, and depth of differentiation, variations within the mantle, and lateral and vertical variation within the crust can only be surmised from the limited sample suites,gravity studies,and surface geophysics of the Apollo era.