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At least 19 recordsLinked to original sources
USGS1969

(ORB II-13 (100)) Geologic map of the Maestlin G region of the moon, Lunar Orbiter site II P-13, Oceanus Procellarum, including Apollo landing site 5

This map shows the geology in and around potential early Apollo landing site 5 in the lunar equatorial belt. The Maestlin G region is in Oceanus Procellarum, about midway between the crater Kepler to the northeast and Flamsteed to the southwest. Terra materials occur only in the northeast corner of the region. Dark mare covers the remainder, and the entire region is crossed by rays from Kepler. The general geology of the larger Kepler region was mapped at a scale of 1:1,000,000 from telescopic photography (Hackman, 1962), and a 1:25,000 geologic map has been prepared of the landing site in the central part of the region (Titley and Trask, 1969).

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USGS1971

Geologic map of the Wichmann CA region of the Moon, Lunar Orbiter Site III P-11, Oceanus Procellarum including Apollo landing sites 4 and 4R

This map shows the geology in and around two potential early Apollo landing sites in the equatorial belt. The Wichmann CA region is in the Oceanus Procellarum, south of the equator, approximately 320 km south of the crater Kepler. It is covered by mare material with numerous ridges, low domes, craters, and crater clusters. Relatively few of the craters are larger than 200 m across. Terra material is absent. The relative freshness of the low domes and prominent mare ridges suggest that the mare material here is relatively young. On an earlier, small-scale reconnaissance geologic map of the Letronne region (Marshall, 1963), mare material in the Wichmann CA region was mapped as Imbrian; but Orbiter photographs show that the oldest craters on the surface are relatively young Eratosthenian craters and mare material is now believed to be Eratosthenian.

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USGS1972

Geologic map of the Flamsteed K region of the Moon (Lunar Orbiter site III P-12, Oceanus Procellarum)

The Flamsteed K region is in the southern part of Oceanus Procellarum , approximately 60 km (kilom eters) north of the crater Flamsteed and 330 km southwest of the crater Kepler. The region was photographed by Lunar Orbiters I and III ; it includes the landing site of Surveyor I and a potential early Apollo landing site. The area is included in a 1:1,000,000-scale map by Marshall (1962).

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USGS1971

Geologic map of the Lansberg P region of the Moon Lunar Orbiter Site III P-9, Oceanus Procellarum including Apollo landing site 7 (Apollo 12)

The Lansberg P region lies within a lowland area between Mare Cognit um and the main part of Oceanus Procellarum , about 135 km due south of the crater Reinhold. The Apollo 12 landing site is in the west-central part of the region and has been mapped in detail by Cannon (1969) . Although the entire region is covered by cratered and rayed mare materials, the mare is almost entirely surrounded by the terrae and is probably relatively thin . Superposed on the mare are two rays from the crater Copernicus, many individual craters, and crater clusters.

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USGS1968

Geologic map of Lunar Orbiter site III P-11, Oceanus Procellarum south of equator

This map shows the geology of Lunar Orbiter site III P-11 within which lies landing ellipse West Two, a potential early Apollo landing site in the lunar equatorial belt. The area is in Oceanus Procellarum, south of the equator, approximately 320 km south of the crater Kepler. It is covered by mare material and the evenness of the mare surface is broken only by mare ridges and some low domes. Relatively few of the superposed impact craters are larger than 200 m across. Terra material is absent.

Open-File Report↗
USGS1972

Photogeology: Part S: mare ridges and arches in southern Oceanus Procellarum

Low-relief mare features such as ridges and arches are best studied by using stereoscopic photographs taken at low Sun angles. Apollo 16 metric camera photography of the southern Oceanus Procellarum east of Letronne Crater reveals a diversity of subtle features (fig. 29-125) and adds significantly to an understanding of the forms of mare ridges and arches their relative ages, and their association with fractures and sinuous rilles.

Book chapter↗
USGS1977

Topography, structure, and mare ridges in southern Mare Imbrium and northern Oceanus Procellarum

The gross topography in southern Mare Imbrium and northern Oceanus Procellarum correlates with the buried structure and deposits of the Imbrium Basin and its rim, and many of the mare slopes may be depositional and reflect the pre-existing major features of the basin. Post-depositional, local distortion of the mare surface, however, is present and in many places associated with mare ridges. Many mare ridges are concentric to the Imbrium Basin suggesting that they are influenced by basin structures. Morphologic diversity of mare ridges suggests that not all have the same origin, and volcanic activity took place along some of them. Most mare ridges are associated with faults. The faults could be reverse and associated with a shrinking of the moon, however, some ridges parallel slopes and could be interpreted as decollement thrust faults along gliding horizons or as vertical faults caused by differential gravitational settling along lines that separate areas that are thinly flooded on topographic highs from areas that are thickly flooded in adjacent lows.

Conference Paper↗
USGS1967

(LAC-38) Geologic map of the Seleucus quadrangle of the moon

The Seleucus quadrangle lies in the northwestern part of the Oceanus Procellarum , a large mare of irregular shape in the western part of the earthside hemisphere of the Moon. Material of the mare occupies most of the quadrangle. Craters ranging from 1 to 44 km in diameter are scattered over the smooth mare surface; in addition, a few isolated hills and ridges rise above the mare. In the east-central part of the quadrangle, the Aristarchus plateau (informal name ) slopes gently westward and merges with the surrounding surface of Oceanus Procellarum . The plat eau is also known for its reddish color and light absorption properties (Wood, 1912), and areas where occasional reddish glows have been seen (Greenacre, 1965).

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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 Rumker Quadrangle of the Moon

The Rumker quadrangle, in the northwest quadrant of the Moon, is adjacent to the western rim of the multi-ring Imbrium basin and to Sinus Iridum , a large (220 km diameter) mare-filled crater. Both of these great depressions were probably formed by impa c t, as indicated here and elsewhere on the Moon by the characteri stic form, distribution, and texture of surrounding materials and structures. The Imbrium b asin and Iridum crater were filled by mare mat erials during the Imbrain and Eratosthenian Periods. In this quadrangle, the widespread ejecta blanke t of the Imbrium basin, as well as the basin’s concentric ridges and mountain rings, has largely been buried by terra materials of mixed origin and by ejecta from Iridum and numerous smaller impact craters. These materials , together with some terra units of probable volcanic origin, make up the highland terrain. Mare materials of Oceanus Procellarum cover part of t his westward-sloping highland shelf that separate it from the Rumker Hills, an isolated plateau surrounded by the mare. No visible discontinuity distinguishes mare material of Oceanus Procella rum from those in the Imbrium basin, both of which contain several units having similar albedo and color. Parts of the mare are very dark and smooth and appear relatively young, and parts of the terra contain many diverse landforms of Imbrian and younger age that appear to be volcanic . This region may therefore have been more active internally during late stages of lunar history than many others on the near side.

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