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At least 19 recordsLinked to original sources

Hydrography of the Gulf of Maine and Massachusetts Bay, data report for R/V OCEANUS cruise 181, 5-15 February 1987

This report presents hydrographic data obtained on R/V OCEANUS Cruise 181 from February 5-15, 1987. The hydrographic measurements (pressure, temperature, salinity, oxygen, beam attenuation, phosphate, silicate and nitrate/nitrite) were obtained in Georges, Jordan, and Wilkinson Basin in the Gulf of Maine and directly east of Boston across Massachusetts Bay as part of a study of currents and sediment transport in this region (figure 1). During Cruise 181, a total of 95 hydrographic profiles were obtained by means of a conductivity-temperature-depth (CTD) profiler. Stations are numbered sequentially and station information is tabulated in table 1. The stations were arranged in ten transects (figure 1). Section 1 was across the Great South Channel and section 7 was across the Northeast Channel--the two main oceanic entrances and exits of the Gulf of Maine. Section 2 was along a saddle (Rodgers Pass) separating Wilkinson Basin from Georges Basin. Sections 3,5, and 10 were across different regions of Wilkinson Basin and all intersected at the longterm mooring site W1 in the center of Wilkinson Basin; section 8 was a dog-leg section through the southern portion of Jordan Basin; and sections 6 (east-west) and 9 (north-south) were within Georges Basin. A severe winter storm (see table 2 and 3) occurred between February 9 and 10 and work was stopped while the OCEANUS rode out the storm in Cape Cod Bay and repaired storm damage. Section 4 across Massachusetts Bay and section 5 across Wilkinson Basin, were repeated twice, once before the storm (sections 4a and 5a) and once after the storm (sections 4b and 5b).

Maine, Massachusetts↗

(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).

IMAP↗

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.

IMAP↗

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).

IMAP↗

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.

IMAP↗

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↗

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↗

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↗