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Lunar geology is mapped on the basis of the principles of stratigraphic sequence. Superposition relations are determined and crater morphologies compared. The sequences of geologic events can then be reconstructed and stratigraphic units can be placed in the established lunar time-stratigraphic system (Shoemaker, 1962; Shoemaker and Hackman, 1962, McCauley, 1967; and Wilhelms, 1970). The age of a crater is determined from several lines of evidence, but particularly from the morphologic criteria discussed by Pohn and Offield (1970) , who studied crater morphologies on Lunar Orbiter photographs and correlated morphologic stages with the lunar time-stratigraphic system (Offield and Pohn, 1970; Offield, 1971). Particularly...
The brightly rayed crater Coperincus, one of the most familiar features of the Moon served as the type example of an impact crater in Shoemaker's (1962) classic analysis. This map shows the geology of the crater as interpreted in photographs taken by Lunar Orbiter V. A geologic map at 1:1000000 scale showing the regional setting of Copernicus and the extent of the rim deposits and satellite craters was prepaid from telescopic observations by Schmitt, Trask, and Shoemaker (1967).
Basic information about the planetary surface of the Kuiper quadrangle is provided by three sequences of high-quality photographs designated Mercury I, II, and II, obtained during the incoming phases of three encounters of the Mariner 10 spacecraft with Mercury. Mercury I includes 75 whole-frame photographs of the Kuiper quadrangle; Mercury II, 13 whole-frame photographs; and Mercury III, 70 quarter-frame photographs. The photographs include 19 stereopairs in the southern part of the quadrangle. The most distant of the photographs was taken at an altitude of 89,879 km, the closest at an altitude of 7,546 km. Resolution, therefore, varies widely but ranges from about 1.5 to 2.0 km over most of the area.
Mangala Valles are a system of outflow channels cut into Terra Sirenum that appear to originate from a fracture of Memnonia Fossae radial to the Tharsis volcanic center (about 1,800 km to the east).
This map is one in a series of 1:500,000-scale geologic maps prepared to investigate areas on Mars of high scientific interest. The quadrangle contains the source area for Mangala Valles, one of the largest outflow channel complexes on Mars (Sharp and Mali, 1975). Preliminary mapping by Masurksy and others (1986), Simbelman (1988), and Champlan and others (1989, 1991) showed that several episodes of channel formation and deposition may have occurred in association with Mangala Valles. To elucidate the complex history Mangala Valles and the general geology of the area surrounding their source, the detailed photogeology of the MTM -20147 quadrangle is presented here.
The Systematic mapping of lava flow units in the Tharsis region has been compiled into a series of 16 maps at 1:2,000,000 scale. This work provides information on the sources and areal extent of the lava flows, on their eruptive sequences and relative ages, and on relations between the flows and geologic structure in the largest, most active tectonic and volcanic province on Mars. Some of the maps were made from controlled Viking photomosaics published as quarter quadrangles in the Atlas of Mars Topographic Series (U.S. Geological Survey, 1979) and tied to the Viking control net. Where these photomosaics were not available, larger scale catalog photomosaics tied to the Mariner 9 control net were used. These maps...
The Systematic mapping of lava flow units in the Tharsis region has been compiled into a series of 16 maps at 1:2,000,000 scale. This work provides information on the sources and areal extent of the lava flows, on their eruptive sequences and relative ages, and on relations between the flows and geologic structure in the largest, most active tectonic and volcanic province on Mars. Some of the maps were made from controlled Viking photomosaics published as quarter quadrangles in the Atlas of Mars Topographic Series (U.S. Geological Survey, 1979) and tied to the Viking control net. Where these photomosaics were not available, larger scale catalog photomosaics tied to the Mariner 9 control net were used. These maps...
The Systematic mapping of lava flow units in the Tharsis region has been compiled into a series of 16 maps at 1:2,000,000 scale. This work provides information on the sources and areal extent of the lava flows, on their eruptive sequences and relative ages, and on relations between the flows and geologic structure in the largest, most active tectonic and volcanic province on Mars. Some of the maps were made from controlled Viking photomosaics published as quarter quadrangles in the Atlas of Mars Topographic Series (U.S. Geological Survey, 1979) and tied to the Viking control net. Where these photomosaics were not available, larger scale catalog photomosaics tied to the Mariner 9 control net were used. These maps...
The Amazonis quadrangle lies within the northern sparsely cratered hemisphere of Mars (Carr and others, 1973). The dominant structural and physiographic features of the quadrangle are low featureless plains (Amazonis Planitia) in the center third of the quadrangle, the western flanks of the large volcanic construct, Olympus Mons, and its associated aureole deposits (Lycus Sulci), which lies on the eastern slopes of the plains, and an area of rough knobby terrain along the west edge of the quadrangle. The central plains descend northward into the circumpolar lowlands (Arcadia Planitita, Vastitas Borealis) and rise southward where they are bounded by the cratered terrains of the equatorial region of Mars.
The area shown on this map includes layered polar deposits and residual polar ice, as well as some exposures of older terrain. Howard and others (1982) noted that an area (at lat 84.8 S., long 356 W.) near a 23-km diameter impact crater (Plaut and others, 1988) appears to have undergone recent deposition, as evidenced by the partial burial of secondary craters. Herkenhoff and Murray (1990a) mapped this area as a mixture of frost and defrosted ground and suggested that the presence of frost throughout the year stabilizes dust deposited in this area. This quadrangle was mapped using high-resolution Mariner 9 (table 1) and Viking Orbiter images in order to study the relations among erosional, cratering, and depositional...
This map shows the geology in and around potential early Apollo landing site 1 in the lunar equatorial belt. The Maskelyne DA region, at the southeastern edge of Mare Tranquillitatis, is in an area transitional between mare and terra. Patches of typical terra material occur on northwest-trending ridges, and typical heavily-cratered mare material occurs only in the east-central part of the region. The terrain in the rest of the region, including the potential landing site, is exceptionally smooth and deficient in craters more than 50 m (meters) in diameter. A large cratered dome, possibly indicative of late-stage volcanism, occurs in the southern part of the region. Telescopically, the terrain over most of the region...
This report includes the first substantive body of in situ density, bearing strength, shear strength, and moisture content data measured by Project personnel. Emphasis in this fiscal year's measurements was on low-density materials since available data suggest that the upper meter or so of the lunar surface consists of low-density material.
These suggestions are largely a result of two closely allied factors: first, a tape recording--either direct or one made via radio--should enable· a field geologist to record many more observations per unit time than can be made in a notebook. The observations should be to the point, but there is no reason for them to be cryptic and so potentially ambiguous to another person. Second, persons in a data facility usually have to form a mental image of the scene being described by the field man in order to understand and to plot the data. The field man therefore has to describe objects by some logical systematic procedure.
Cinder Lake symbology, unit descriptions, and ideas tested at Cinder Lakes and Verde Valley, northern Arizona.
The Beethoven quadrangle is located in the equatorial region of Mercury, in the center of the imaged area. Most pictures of the quadrangle were obtained at high sun angles as the Mariner 10 spacecraft receded from the planet. Images in the northeastern part of the quadrangle are very poor to unusable. Another difficulty in mapping is the poor match in topographic bases between Beethvoen and adjacent quadrangles. Mismatches are especially common along the borders withthe Kuiper and Discovery quadrangles to the east and southeast.
Categories: Data;
Types: ArcGIS REST Map Service,
ArcGIS Service Definition,
Downloadable,
Map Service;
Tags: 1:5,000,00,
Geological and Geophysical,
Mariner10,
Mercury,
Planetary sciences,
This map sheet is one of a series covering that part of the surface of Mercury that was illuminated during the Mariner 10 encounters. Planimetric control is provided by photogrammetric triangulation using Mariner 10 pictures (Davies and Batson, 1975). Discrepancies between images in the base mosaic and computed control-point positions appear to be less than 5 km. No attempt was made to resolve discrepancies in feature positions on this sheet and those on the Kuiper (H-6) quadrangle to the north and the Bach (H-15) quadrangle to the south. The latter sheets were controlled by an earlier, more preliminary net.
Categories: Data;
Types: ArcGIS REST Map Service,
ArcGIS Service Definition,
Downloadable,
Map Service;
Tags: 1:5,000,000,
Geological and Geophysical,
Mariner10,
Mercury,
Planetary sciences,
Mars presents two different terrains, a highly cratered surface that lies mostly in the southern hemisphere and sparsely cratered plains that lie mostly in the northern hemisphere. The cause of the dichotomy is a still unsolved fundamental problem of Martian geology, analogous to the problem of continents and ocean basins in terrestrial geology. The present features of the plains in particular reflect a varied history in which superficially similar landforms may have had very different origins. The Lunae Palus quadrangle is occupied mainly by plains and their variety is perhaps more evident than elsewhere. This map demarcates units inferred to have different geologic histories on the basis of their appearance in...
This dataset contains two feature classes - contacts and map units - digitized from the Atlas of Mars 1:5,000,000 Geologic Series Map Arabia Area (1977). Geologic structures have been omitted.
Monthly report to show updates on personnel and conferences and scientific meetings. Includes unpublished works and works in progress.
Most images used in mapping the geology of the Shakespeare quadrangle were taken during the near-equatorial first pass, with close encounter on teh dark side of the planet. The second, south-polar pass did not image the Shakespeare quadrangle at high resolution. High-resolution images of small areas within the quadrangle were also obtained during the third pass, when the spacecraft was on the near-encounter north-polar trajectory. Because the spacecraft viewed the same areas from different positions during the first and second passes, stereoscopic pictures are available for certain areas of the southern hemisphere; however, such pictures are not available for the Shakespeare quadrangle. This map includes a strip...
Categories: Data;
Types: ArcGIS REST Map Service,
ArcGIS Service Definition,
Downloadable,
Map Service;
Tags: 1:5,000,000,
Geological and Geophysical,
Mariner10,
Mercury,
Planetary sciences,
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