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D.E. Stuart-Alexander

Publications and source records attributed to D.E. Stuart-Alexander.

6 recordsLinked to original sources

Geologic map of the central far side of the Moon

This map is one of a series of geologic maps t hat will cover the entire Moon at a scale of 1:5,000,000. The geology of the central far side is compiled largely from NASA Lunar Orbiter and Apollo photographs and Soviet Zond photographs; the discussion and interpretation of geologic units incorporate the geochemical and geophysical data obtained from orbiting s p acecraft. Geologic units are based on the stratigraphic framework established by Shoemaker and Hackman (1962) as subsequently revised (summarized by McCauly , 19 67 ; Wilhelms , 1970; Mutch , 1972; Stuart-Alexander and Wilhelms , 1975). Description of map units is brief because they largely follow units described on the nearside 1:5,000,000 map of Wilhelms and McCauley (1971). The reader unfamiliar with lunar maps, mapping principles, and terminology is referred to that map. Only new units and features or units whose origins are still much in doubt are discussed here.

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Geologic map of the Fracastorius Quadrangle of the Moon

The multi-ringed Nectaris basin ( Hartmann and Kuiper, 1962) dominates the Fracastorius quadrangle. The basin is 840 km across as measured from the outermost ring and lies athwart four quadrangles. Frac astorius , the southeastern quadrangle , straddles the three rings of the basin (fig. 1 ). In this quadrangle most pre- Imbri an structures and many depositions were formed by the Nectaris impact. Furthermore, the emplacement of many younger deposi ts was controlled by basin structures and locally by probable multi-ring structures related to the Fecunditatis basin center ed northeast of the quadrangle. Other geologic features in the area include diverse mantling deposits and both primary impact craters and secondary impact craters produced by ejecta from distant impacts .

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Geologic map of the Rheita Quadrangle of the Moon

Photographs returned by unmanned Lunar Orbiters have contributed greatly to the current lunar geologic mapping program. This is particu larly true for quadrangles near the limbs, such as Rh eita in the southeast earthside quadrant. The new data and revised in terpretations amend the geologic framework established by earlier workers (Shoemaker (1962) and Shoemaker and Hackman (1962) applied basic stratigraphic principles to set up a lunar time scale; McCauly (1967) summarized changes made in he next five years of study; Wilhelms (1970) compiled all the telescopic refinements and additions to the original framework) . Detailed studies of crater morphologies from Lunar Orbiter photographs ( Pohn and Offield , 1970) permit the placement of most craters within the time- stratigraphic systems ( Offield and Pohn , 1970 : Offield , 1971). Other advances in understanding lunar processes included establishing the sequence of formation and features of large, multiringed basins ( McCauly , 1968; Stuart-Alexander and Howard, 1970) and criteria for distinguishing between impacts and possible volcanic craters (McCauly,1968).

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