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Material exposed on the surface of the moon is heterogenous. The albedo and other physical characteristics that have been determined with the use of optical and radio telescopes vary from one part of the moon from another, and the variations are partially correlated with differences in topography. Discontinuities in the areal variation permit the surface material to be divided up into map units, each exhibiting a limited range of topographic characteristics. Each map unit is further characterized by a distinctive pattern of distribution, and the patterns of certain units are in places superimposed on the patterns of other units. From the relations of superposition it is possible to determine the sequence in which...
The geology of the Thaumasia region (fig. 1, sheet 3) includes a wide array of rock materials, depositional and erosional landforms, and tectonic structures. The region is dominated by the Thaumasia plateau, which includes central high lava plains ringed by highly deformed highlands; the plateau may comprise the ancestral center of Tharsis tectonism (Frey, 1979; Plescia and Saunders, 1982). The extensive structural deformation of the map region, which is without parallel on Mars in both complexity and diversity, occurred largely throughout the Noachian and Hesperian periods (Tanaka and Davis, 1988; Scott and Dohm, 1990a). The deformation produced small and large extensional and contractional structures (fig. 2,...
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...
Apollo 16 geology training schedule for January, 1972.
This is a collection of tables and graphs showing information on sample collection rates and types and photography rates.
This is a revision of a previous field trip schedule. Date range for training is May 24,1972, to November, 1972.
This is a memo containing the proposed schedule for the Apollo 17 geology field trip including dates and locations.
Telefax Detailing the NV00 Support Needed for NTS Field Exercise
The Oxia Palus quadrangle contains three distinct geologic provinces: (1) an elevated cratered plateau that occupies three-fourths of the quadrangle and is similar to much of the southern hemisphere of Mars; (2) the low, relatively featureless Chryse Planitia in the northwest corner; and (3) a complex province of chaotic terrain and immense channels or valleys that divides the plateau an determinates at Chryse Planitia. Generally, the oldest geologic units occur in the plateau province and the youngest in Chryse Planitia. Discovery by Mariner 9 of the channels, the four largest of which are given neames meaning “Mars” in Akkadian, Sumerian, Anglo-Saxon, and Greek (west to east), renews the possibility of water and...
The Thaumasia quadrangle lies on the south flank of the Tharsis dome (Hord and others, 1974), a large bulge in the crust of Mars extending more than 5,000 km northward from the center of the quadrangle. This major structure imposes a generally southward slope across the entire quadrangle. Topography along the east-central border of the Thaumasia quadrangle exhibits curved scarps and lowlands concentric with the Argyre basin.
The Valles Marineris region lies east of Tharsis Montes (which extend from lat 12˚ to 16˚., long 101˚ to 125˚). Part of the region is in the midst of a vast plateau bounded on the west and east by Claritas and Nectaris Fossae, respectively; the remainder extends farther east into southern Xanthe Terr and western Margaritifer Terra. Channel trends, stereophotogrammetry, and radar altimetery indicate that the surface north and east of the canyons slopes toward Chryse Planitia (centered at about lat 25˚ N., long 45˚). Within the broad Valles Marineris region, three distinct physiographic provinces are recognized (fig. 1): (1) the Noctis Labyrithus province, consisting of a high plateau cut by a network of structurally...
This map is one in a series of 1:500,000 scale geologic maps initiated by the National Aeronautics and Space Administration to investigate areas of particular scientific interest on Mars, The West Mangala Valles area merits detailed geologic study because it contains several small channels whose ages can be determined relative to geologic units that range in age from early (Noachian) to late (Amazonian) Periods of martian history. Because the small channels are of three ages and channels of each age are of a geomophic type unique to that age, their study increases our understanding of the continuity of fluvial processes in the evolutionary history of Mars. For these reasons, part of the area is a proposed site for...
The surface of the Moon is heterogeneous both on a regional and a fine scale. The geologic mapping of this surface is similar in principle to the geologic mapping of the Earth's surface and depends on the discrimination of similarities and differences between materials and features at different points on the surface. Differences from area to area in characteristic topographic forms and in such physical properties as albedo indicate that the areas are underlain by materials of different nature and have formed under different processes. The units shown on the map are analogous to stratigraphic units adopted for mapping terrestrial geology in that they are bodies of rock with a limited range of properties and age and...
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.
Mariner 10 photographic coverage was available for only the eastern two-thirds of the Tolstoj quadrangle. Image data from three Mariner 10 encounters with Mercury were used in mapping the quadrangle.
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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