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The Magellan spacecraft orbited Venus from August 10, 1990, until it plunged into the venusian atmosphere on October 12, 1994. Magellan had the objectives of (1) improving knowledge of the geologic processes, surface properties, and geologic history of Venus by analysis of surface radar characteristics, topography, and morphology and (2) improving knowledge of the geophysics of Venus by analysis of venusian gravity. The Magellan spacecraft carried a 12.6-cm radar system to map the surface of Venus. The transmitter and receiver systems were used to collect three datasets: synthetic aperture radar (SAR) images of the surface, passive microwave thermal emission observations, and measurements of the backscattered power...
The Galindo quadrangle (V-40; centered at lat 12.5° S., long 255°) was geologically mapped at 1:5,000,000 scale under the Venus Data Analysis and Venus Geologic Mapping Programs as part of a project focused on the study of venusian geologic terrains containing assemblages of coronae, arachnoids, and novae; these are enigmatic circular features perhaps related to hot-spot volcanism. Mapping of the quadrangle indicates most coronae are related to extension zones, and some aligned coronae and corona-like features show systematic variations in age. Standard photogeologic techniques were used to map the geology on the synthetic aperture radar (SAR) backscatter mosaic of V-40, which was generated by the radar image data...
The area of MC-28 is centered at the east edge of the Hellas Planitia (Hellas basin and surrounding plains) within densely cratered terrain that covers more than half the surface of Mars (Carr, 1973). The deepest part of the basin lies 4-5 km below the surface of the cratered terrain (Hanel and others, 1972). An irregular band of mountain and knobby material about the eastern margin of the basin and broad bands of mantled rough material on the floor of the basin represent ejecta from this very old impact. The vast, gently sloping, featureless eastern and southern part of Hellas Planitia, shown on the Shaded Relief Map of Mars (U.S.G.S., Atlas of Mars, MM 25M IR, 1972), is probably the result of extensive volcanic...
A collection of materials created by Astrogeology and/or their NASA-funded collaborators, primarily in support of the Apollo missions.
The main idea behind this slide presentation is to develope a general philosophy on: 1) lunar impact cratering processes, 2) characteristics of impact craters and ejecta as a function of target material and, size, 3) the effects of layered targets on impact crater morphology, and 4) illustration of the above for lunar sites.
Enclosed are the seismic profiles and a plan of the seismic lines at the new Cinder Lake Crater Field in Yavapai county. Along the East-West line the upper layer is made up of 3.5 feet of cinders on the top and then becoming mixed with clay t o a depth of 7.5 to 11.0 feet below the surface. Beneath this is a 10 to 20 foot thick layer of denser cinders or some other unconsolidated material. The third layer, with velocities from 5100 to 5950 ft. per sec., is probably a lava similar to that at Kona-A.
The Bach region encompasses the south polar part of Mercury poleward of lat 65° S. About half of hte region was beyond the terminator during the three Mariner 10 encounters and hence not visible. The entire mapped area was covered by near-vertical photography from the second encounter, and the eastern part, from long 15° to about 110°, was covered by oblique photography from the first encounter.
Categories: Data;
Types: ArcGIS REST Map Service,
ArcGIS Service Definition,
Downloadable,
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The original geologic maps of the Taurus-Littrow region (I-800) were published in 1972 as two map sheets (1:250,000 and 1:50,000) in a Transverse Mercator projection to support the Apollo 17 mission, the sixth and final crewed mission to land on the Moon (December 7 – 19, 1972). These renovated versions of the 1:50k and 1:250k maps represent a best effort to capture and preserve the fidelity of the original mapping effort in an interactive digital format. These maps are not updated versions or reinterpretations of the original geologic maps which were based on Apollo 15 metric photographs, but spatial adjustments to a Lunar Reconnaissance Orbiter (LRO) Wide Angle Camera (WAC) basemap to make the maps more compatible...
This 1:5,000 scale geolgic map is one of a series made from photographs transmitted by the Ranger VIII spacecraft. The Sabine EB region, in the southwestern part of Mare Tranquillitatis, is adjacent to the Sabine DM area, which was mapped at a scale of 1:50,000 by Trask (1969). The geology of parts of the map area was evaluated by H.H. Schmitt (in Shoemaker, 1966 p. 326-331) and Kuiper, Stroms and LePoole (1966, p. 91-93, p. 115-117). For this study Lunar Orbiter II photographs were used to fill in details on the South and West sides of the map area where the Ranger data are poor. One of the main objectives of the study was to asses the applicability of lunar geologic mapping at this scale and resolution.
The Arcadia quadrangle of Mars contains three distinct geologic provinces: (1) the 1000-km-diameter shield volcano of Alba Patera, which occupies the southwestern quadrant; (2) the complex Tempe province, which comprises a number of younger volcanic and sedimentary blanket deposits over an ancient, highly cratered crust forming a plateau in the southeastern quadrant; and (3) a plains province, consisting of northern wind-swept, cratered plains and some younger subpolar deposits in the northeast corner of the quadrangle, plus less cratered plains surrounding much of the Tempe and Alba regions. The plateau, informally named the Tempe Plateau and part of the proposed formal term Tempe Terra, is separated from the main...
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 geologic map of Ophir and central Candor Chasmata is one of a series of 1:500,000 scale maps prepared for areas on Mars that are of particular scientific interest and may serve as potential future landing sites. This map is also part of a set that includes east Candor Chasma, west Candor Chasma, and Melas Chasma. The geologic interpretations are based dominantly on medium- and high-resolution Viking images, many of them stereoscopic, and supplemented by lower resolution apoapsis and other color images. A strip of very high resolution stereoscopic images (~20 m/pixel) crosses the central part of the quadrangle from northwest to southeast and served to clarify detailed relations not obvious on other images. A...
Most of the Cebrenia quadrangle (lat 30° to 65° N., long 180° to 240° W.) is in the circumpolar plains of Mars. Craters from an early episode of intense bombardment have been largely obliterated by later volcanism, tectonism, erosion and sedimentation by wind and water, and by circumpolar glacial and periglacial processes. South of 47° N. the plains are dissected by numerous channels, most of which drained off abroad volcanic upland near the southern border of the quadrangle. The impressive Elysium volcanoes cap the crest of this upland; their northernmost member, Hectates Tholus, lies within the Cebrenia quadrangle.
The Plato quadrangle in the north-central part of the Moon lies within a series of concentric depressed and raised rings surrounding the Imbrium basin, the center of which lies about 335 km southwest of Montes Teneriffe. The innermost raised ring is marked by isolated ridges and peaks within Mare Imbrium itself, including in the Plato quadrangle Montes Recti and Teneriffe. The band of terra including Montes Aples forms part of the second and most prominent raised ring, immediately encircling Mare Imbrium. Mare Frigoris is part of the succeeding depressed ring and the terra in the north of the quadrangle part of the third raised ring. It is believed that the Imbrium basin and other multi-ringed basins on the Moon...
Evaluation of the MSFC Facsimile Camera System as a Tool for extraterrestrial geologic exploration
Drill Core Log of Cinder Lake (in Yavapai county) Collected in September 10-17, 1968. The driller is listed as Justus.
Material exposed on the surface of the moon is heterogeneous. 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 to another, and the variations are partially correlated with differences in topography . Discontinuities in the areal variation permit the surfaces material to be divided 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...
Material exposed on the surface of the Moon is heterogeneous. 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 to another, and the variations are partially correlated with differences in topography. Discontinuities in the areal variation permit the surface material to be divided into map units, each exhibiting a limited range of photometric properties associated with 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 superpositon...
Formation of the three major impact basins apparently influenced the early geologic development of the petavius quadrangle. First of these was Fecunditatis, whose outer structure probably underlies much of the terrae. Large degraded craters such as Snellius formed subsequently, followed by the Nectaris impact basin and its associated radial features, including Vallis Snellius, Crisium may be youngest of the three basins and its represented in this quadrangle by the terminus of a secondary crater chain and by ejecta forming at least parts of the smooth and hummocky materials.
The Tharsis quadrangle lies within the sparsely cratered hemisphere (Carr and others, 1973) of Mars. Its geology is dominated by young volcanic features, including both circular constructs and lava plains; little evidence of primitive densely cratered terrain remains. Included are three of the four largest shield volcanoes in the Tharsis province, Olympus Mons, Ascraeus Mons, and Pavonis Mons, together with several smaller shields. The fourth shield, Arsia Mons, lies to the south of the map area, as does Labyrinthus Noctis at the west end of the equatorial canyon system. The terrain within the quadrangle has approximately 25 km of relief with the three shield volcanoes standing 9 to 25 km above the plains, which...
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