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At least 847 records · Page 47Linked to original sources
USGS1972

Geologic map of the Maurolycus Quadrangle of the Moon

The Maurolycus quadrangle , located in the southeastern highlands, includes densely to moderately cratered terrain with many craters larger than 45 km in rim crest diameter . Several appea r to be ancient and may be among the most primitive discernable features on the lunar surface. Major stratigraphic units consist of the Janssen Formation, hummocky terra and pitted plains materials, and e xtensive clusters of bowl-shaped craters. Two of these units, hummocky terra and pitted plains , a re probably volcanic whereas the Janssen Formation and bowl-shaped craters appear t o have been formed by ejecta from the multi-ringed Nectaris and Imbrium basins outside the quadrangle.

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USGS1972

Geologic map of the Tycho Quadrangle of the Moon

The Tycho quadrangle is centrally located in the southern half of the earthside hemisphere of the Moon. The area is characterized by a high density of craters, the largest of which – Stofler – is about 140 km in diameter. The northern and eastern parts if the quadrangle are dominated by plains ( pIp , Ip ) and hilly terra ( IpIt ) units of regional extent , and the western part by the crater Tycho and its ejecta blanket. Structural features probably associated with the Imbrium basin to the north and Orienta le and Humorum basins to the northwest are present, although blanketing units related to these basins are not recognized.

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USGS1972

Geologic map of the Aristoteles Quadrangle of the Moon

The Aristoteles quadrangle, located on the northeastern periphery of the Imbrium basin on the near side of the Moon, consist of four physiographic provinces : a northern mountainous belt, chiefly of lineated crater rims and other lineated terra; a middle-northern belt covered by mare material of Mare Frigoris ; and a southern belt composed of mountainous material of diverse characteristics. The crater Aristoteles and its ejecta blanket dominate the southwestern part of the quadrangle, and ejecta from the crater Hercules (outside the quadrangle) covers a small part of the southeastern corner. Other promin ent craters are Democritus, C. Mayer, Gartner, and Kane. Two probable centers of tectonism and volcanism are present in the southern mount ainous belt.

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USGS1973

Geologic map of the Langrenus Quadrangle of the Moon

The Langrenus quadrangle is on the east limb of the lunar nearside, at the southeast margin of Mare Fecunditatis . The crater Lan grenus , about 140 km in diameter, is the most prominent feature. Rugged terra materials, scattered by craters of various sizes and ages, occupy much of the east half of the map area, and smooth mare materials in the Fecunditatis basin dominate the west. Mare Spumans and other irregular maria in the northeast are part of a belt of such maria concentric with Mare Crisium , which is centered approximately 500 km north of the quadrangle.

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USGS1973

Geologic map of the Grimaldi quadrangle of the Moon

The Grimaldi quadrangle lies at the southwest margin of Oceanus Procellarum about 1,000 km east of Orientale, the youngest o f the lunar multi-ringed basins. The distal ends of the ejecta blanket surrounding the Orient al e basin partly covers the western third of the quadrangle. The relatively small, two-ring Grimaldi basin is in the northwest corner of the quadrangle, and the Humorum basin l ies about 750 km to the southeast. A vestigial multi-ring basin mostly engulfed by mare appears to control the distribution of terra and mare along the southwest margin of Oceanus Procellarum ; the craters Hansteen and Billy are on a northwe s t-trending topographic high which represents part of the ring system of this basin. Terra materials of distinctive texture, apparently unrelated to multi-ring basins and probably of volcanic origin, occupy the central parts of the quadrangle.

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USGS1973

Geologic map of the Byrgius Quadrangle of the Moon

The By rgius quadrangle, at the western edge of the near side, lies in the terra southwest of Oceanus Procellarum between the Humorum and Orientale basins. Structures and deposits related to the Orientale basin, which is younger than the Humorum basin (Hartmann and Kuiper, 1962 ), dominate the southwestern half of the quadrangle . The northeastern half is dominated by mantling deposits that are older than Orientale ( Imbrian ) and younger than Humorum (pre- Imbrian ), which lies mostly outside the zone of reco gnizable Orientale-related deposits or structures. These main subdivisions are visible on the albedo map of the Moon ( Pohn and Wildey , 1970) , the northeastern one having generally the lower albedo . The older units throughout the quadrangle have complex topography, probably formed mostly intersecti ng, degraded craters .

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