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The surface of the moon is heterogeneous. Surface materials are classed on the basis of telescopic observations into units each having a limited range of physical properties such as topography, visible under low-illumination and albedo, the reflectivity under full-Moon illumination. Such units are considered analogous to the rock-stratigraphic formations of terrestrial geology. By application of the principles of superposition and intersection, these rock units are arranged in order of relative age and grouped into time stratigraphic units. Following terrestrial contention, the major time-stratigraphic units are designated systems, and their subdivisions, series; corresponding to these units are periods and epochs...
The Sinus Iridum quadrangle includes the northwestern sector of Mare Imbrium, the Sinus Iridum embayment, the arcuate Montes Jura which partly surround Sinus Iridum, and several terra islands in the mare such as the Montes Teneriffe, Montes Recti, and C. Herschel. Mare Imbrium occupies a complex depression or basin consisting of an inner basin and several outer concentric troughs seperated by raised rings (Hartmann and Kuiper, 1962). The center and much of the inner basin part of the first raised ring, and part of the first trough lie within and quadrangle. The terra islands are exposed parts of the first raised ring, which is approximately 670 km in diameter. Sinus Iridum embays a simpler and smaller structure,...
The geology of the Rhetia quadrangle is dominated by deposits and structures resulting from the event that produced the multi-ringed Nectaris basin, an 840-km (measured from the outermost mountian ring) circular basin that lies northwest of the quadrangle (Hartmann and Kuiper, 1962). The deposits (presumably ejecta) and their structures, which include the Vallis Rhetia and other crater-trough valleys (Baldwin, 1963, p 317-318; Hartman, 1964), give a northwest "grain" to the area; younger and less abundant lineaments trend mainly northeast and seem to reflect the lunar grid (Fielder, 1961; Storm, 1964) rather than the Nectaris event.
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...
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.
The polar deposits on Mars are of great interest because they probably record martian climate variations (Thomas and others, 1992). The area shown on this map includes polar layered deposits with distinct low-albedo features and a sharp boundary between the layered deposits and the moderately cratered unit that forms the floor of Chasma Australe. Detailed mapping of this quadrangle was undertaken to further investigate the geologic relations between the albedo features and the layered deposits and to better constrain the recent geologic history of the south polar region. Dark dunes in the north polar region appear to be derived from erosion of the layered deposits, but the source of dark material in the south polar...
This map is one of a series prepared from photographs transmitted by Ranger IX (Jet Propulsion Lab, 1966, pls A56-58, B70-82). It depicts the geology of some 724 sq km in the northeast part of the floor of Alphonsus (Diameter about 115 km), a typical flat-floored old terra crater or basin with a subdued rim. Similar basins abound in the south central terrae of the visible hemisphere and on the far side of the Moon. Alphonsus is of particular interest, however, because of a well developed interior rille system and associated dark-halo craters.
The surface of the Moon is heterogeneous. Surface materials are classed on the basis of telescopic observations into map units, each having lateral continuity and a limited range of physiographic characteristics and optical properties (mainly polarization and albedo, the reflectivity under full moon illumination). Such units are analogous to the rock-stratigraphic formations of terrestrial geology. By application of the principles of superposition and intersection, these formations are arranged in order of relative age and grouped into time-stratigraphic units. Following terrestrial convention, the major time-stratigraphic units are designated systems, and their subdivisions series; corresponding to these are periods...
The surface of the moon is heterogeneous. The differences from area to area of characteristic topographic forms and of physical properties such as albedo (reflectivity under full-Moon illumination) indicate that the materials underlying the surface vary from one area to another and that different processes have operated in the development of the surface. In lunar geologic mapping, areas are delineated that, as far as possible, are analogous in terrestrial mapping to the areas of outcrop of stratigraphic units - bodies of rock whose limited range of lithology and age and relatively simple geometric form indicate formation under a common set of conditions. For the moon, at the present time, physical properties that...
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