Geology topics
Research about Moon
Source-linked reports with geographic coverage including Moon.
(RLC-15) Geologic map of the Alphonsus GA region of the moon
This ma p is one of a series prepared from photographs transmitted by R anger IX (Jet Propulsion L ab ., 1966. , pls. A56-A58, B70-B82). It depicts the geology of some 724 sq km in the northeast p a rt of the floor of Alphon s us (diameter about 115 km), a typical flat-floored old terra crater or basin with subdued rim. Similar basins abound in the south-central tarrae of the visible hemisphere and on the far side of the Moon. Alphonsus is of particular inte re st, however, because of a well-developed interior rille system and a ssociated dark-halo craters.
(LAC-11) Geologic map of the J. Herschel quadrangle of the moon
Lunar surface materials are classed into units on the basis of visual observations and data from telescopic and Lunar Orbiter photographs. Each unit has a distinctive range of physical characteristics, such as topography and albedo (re flectivity under full-Moon illumination ) , and is considered analogous to a terrestrial rock-stratigraphic formation. These characteristics rather than lithologic properties must, of necessity, suffice to define the units; however, the morphologic nature of most mappable units on the Moon, is , of itself, suggestive of a certain lithologic composition, based on analogous terranes on Earth.
Geologic setting of the lunar samples returned by the Apollo 11 mission
The Apollo 11 LM landed approximately 20 km south-southwest of the crater Sabine D in the southwestern part of Mare Tranquillitatis ( fig. 3-1 ). The landing site is 41.5 km north-northeast of the western promontory of the Kant Plateau (ref. 3-1 ), which is the nearest highland region. The Surveyor 5 spacecraft is approximately 25 km north-northwest of the Apollo 11 landing site, and the impact crater formed by Ranger 8 is 68 km northeast of the landing site.
Geologic map of the Ptolemaeus Quadrangle of the moon
The Ptolemaeus quadrangle is near the center of the lunar disk , in the northern part of the southern highlands . Smooth dark maria border the quadrangle on the west and north, but most of the area is complex, highly cratered terra.
Chapter 3: Television observations from Surveyor VI
Surveyor VI landed on the lunar surface at 01:01:05 GMT on day 314 (November 10, 1967) in the southwestern part of Sinus Medii near the center of the visible face of the Moon. Over 30,000 pictures were transmitted from the spacecraft during the first lunar day of operation. The number of pictures taken by Surveyor VI almost equals the total number of pictures returned from the previous Surveyor missions combined. The pictures were received at the Goldstone, California, Canberra, Australia, and Madrid, Spain, tracking stations of the Deep Space Network.
Surveyor V: Discussion of chemical analysis
Material of basaltic composition at the Surveyor V landing site implies that differentiation has occurred in the moon, probably due to internal sources of heat. The results are consistent with the hypothesis that extensive volcanic flows have been responsible for flooding and filling the mare basins. The processes and products of lunar magmatic activity are apparently similar to those of the earth.
Surveyor V: Television pictures
Surveyor V landed in a small crater, 8.5 meters wide and 12.5 meters long, which was probably formed by drainage of surficial fragmental debris into a subsurface fissure. The lunar surface debris layer is exposed in the walls of this crater. At depths below about 10 centimeters, the debris appears to be composed mainly of shock-compressed aggregates, ranging from a few millimeters up to 3 centimeters in diameter, set in a matrix of less-coherent finer particles. Rocky chips and fragments larger than a millimeter are dispersed as a subordinate constituent of the debris.
(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).
Preliminary geologic map of the Eudoxus Quadrangle of the moon
No abstract available.
Chapter III: Television observations from Surveyor III
Surveyor III landed on the lunar surface at 00:04 GMT, on Day 110 (April 20), 1967, approximately 23 h after local sunrise on the moon. The television camera was turned on about 1 h after touchdown, and 6315 pictures were taken during the remainder of the lunar day. The camera was operated extensively for the first period of lunar visibility from the Goldstone Tracking Station of the Deep Space Network (DSN) and, except on Day 115 (April 25), on each successive Goldstone pass of the moon. During this period, the sun rose from an elevation angle of 11 deg in the east to within 3 deg of the zenith and then sank almost due west of the spacecraft. Many pictures were obtained of the illuminated eastern horizon in the period immediately preceding sunset. In addition to those received at the Goldstone station, some were obtained at the Canberra, Australia, station of the DSN.
Chapter 8: Lunar theory and processes
Significant new information has been provided by Surveyor III's successful landing and operation on the lunar surface; some of the most significant and interesting events are presented here. Pending completion of data reduction and more detailed analysis of the information available from the Surveyor mission, only limited interpretive discussion is included.
Chapter VIII: Lunar theory and processes
Much valuable new information has been provided by Surveyor III ; some of the most significant and interesting events are presented here. Only a limited interpretive discussion is included at this time, pending completion of data reduction and more detailed analysis of information available from the Surveyor mission.
Surface material of the moon
A skeletal fuzz that consists mostly of open space probably covers the moon to a depth of several millimeters or centimeters. The solid part of the fuzz probably consists of randomly oriented linear units, with or without enlarged nodes, which either anastomose in a mesh or are branching.