Distribution and modes of occurrence of lunar anorthosite

We have utilized telescopic near‐infrared spectra and multispectral images of the Moon provided by the Galileo and Clementine missions to determine the distribution and modes of occurrence of pure anorthosite. Anorthosites have now been identified in all portions of the nearside, including the site of the putative Procellarum basin. Anorthosite is associated with the rings of Orientale, Grimaldi, Humorum, Nectaris, Nubium, Mutus‐Vlaq, and Balmer basins. Major portions of the inner rings of Grimaldi, Humorum, Crisium, Orientale, and Nectaris are composed of pure anorthosite. The large spatial extent of these anorthosites appears to rule out an origin in the upper portions of discrete differentiated Mg‐suite plutons. In every instance, the anorthosites were exposed from beneath a shallower near‐surface layer of more pyroxene‐rich material. More mafic material also occurs beneath the pure anorthosite unit. Large expanses of the northern farside exhibit very low FeO values. This region contains abundant anorthosite and stands in stark contrast to the mafic composition exhibited by the interior of the South Pole‐Aitken basin (SPA). The distribution of compositional units on large portions of the lunar farside as well as the southern portion of the lunar nearside appears to be largely attributable to the SPA impact event. The distribution and modes of occurrence of anorthosites clearly indicate that a thick, global layer of anorthosite is present at various depths beneath most portions of the lunar surface. This anorthosite layer dominated the upper portion of the primordial crust and was produced by plagioclase flotation in the global magma ocean.