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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.
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 Beethoven and adjacent quadrangles. Mismatches are especially common along the borders with the Kuiper and Discovery quadrangles to the east and southeast.
A field test held in the Hopi Buttes, Arizona, was planned to test geological, geophysical, and analytical operations and instruments that are of potential use in Apollo Extension Systems lunar surface missions. The test was conducted under "shirt-sleeve" conditions, but potentially useful methods of recording and compiling information during lunar exploration were employed. The test showed that by using specially planned procedures, field and analytical information can be evaluated during field operations and compiled at a location that is remote from the field. It also showed that the more information that is analyzed as operations progress, the more effectively can succeeding operations be conducted. Experience...
When the Apollo astronauts land on the Moon, their precise location will not be known. The real-time geologic mapping planned for the first mission could best be done if the exact position of the landing site were determined. The astronauts may have to find their position, with or without assistance from the Earth-based scientific mission center, before leaving the Lunar Module (LM), and the less time this takes, the more time will be available for exploring the lunar surface.
The original geologic maps of the Apennine-Hadley region (I-723) were published in 1971 as two map sheets (1:250,000 and 1:50,000) in a Transverse Mercator projection to support the Apollo 15 mission, the fourth crewed mission to land on the Moon (July 26 – August 7, 1971). 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 Lunar Orbiter images, but spatial adjustments to a Lunar Reconnaissance Orbiter (LRO) Wide Angle Camera (WAC) basemap to make the maps more compatible with current...
Appendices include the original survey, response data, and collated results related to the Open File Report. Geoscience maps, regardless of target body, are spatial and temporal representations of materials and processes recorded on planetary surfaces (Varnes, 1973; Spencer, 2000). The information and context provided by these maps promote basic and applied research within and across various geoscience disciplines. They also provide an important basis for programmatic and policy decisions (for example, H.R. 2763 – 102nd Congress, National Geologic Mapping Act of 1992). Since 1961, planetary (that is, all solid surface bodies in the Solar System beyond Earth) geoscience maps have been used in nearly every facet of...
Geology training report for the period of 419710820 to 19711231 detailing photos and samples taken by each participant for each part of the exercise.
Geology training report from 19710820 to 19711231 detailing photos taken and samples collected by each participant for each exercise.
The Elysium quadrangle includes part of the vast, relatively low and featureless plains that encircle the subpolar region of Mars immediately north of the more elevated and cratered equatorial belt. The plains are interrupted in the northwest by two large volcanoes, second only in size and youthful appearance to some of the large constructs that form the planet’s most prominent volcanic center in the Tharsis region several thousand kilometres to the east (Carr, 1975). The large irregularity shaped crater Orcus Patera, at the east boundary of the map, closely resembles the lunar crater Schiller but is more than twice as long. A band of knobby, relatively old terrain extends in a broad arc northeastward through the...
The Sinus Sabaeus quadrangle lies in the southern equatorial region of Mars. It is bounded on the north by the equator, on the west by the central meridian, on the south by lat 30° S., and on the east by long 315° W. Three classical regions that have low albedos occur within the quadrangle (Lowell Observatory, 1971): (1) half of Sinus Meridiani occupies part of the northwest corner of the quadrangle; (2) Sinus Sabaeus forms a broad east-west band 180 to 360 km wide across the upper part of the quadrangle along lat 10° S.; and (3) Serpentis Minor occupies the southeast corner. The classical high-albedo regions of Deucalionis Regio and Pandorae Fretum occupy the western and central southern parts of the quadrangle;...
The Memnonia quadrangle lies astride the boundary between heavily cratered and sparsely cratered hemispheres of Mars (Carr and others, 1973). Densely cratered terrain occurs in the southwestern part of the quadrangle. Strips of plains material bound the cratered terrain in both the northern and eastern parts of the quadrangle. There is approximately 3 km of relief across the quadrangle, with the highest elevations in the eastern part. Plains materials of this region are situated along the lower Lacus and Tharsis quadrangles. There is little correlation between terrain type and elevation within the Memnonia quadrangle. In particular, the boundary between cratered terrain and plains for the most part is not marked...
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 Diacria quadrangle lies within the north circumpolar lowlands of Mars (Carr and others, 1973; Scott and Carr, 1978). The dominant structural and physiographic features are low, relatively smooth plains (Arcadia Planitia, Vastitas Borealis) that form the northern two-thirds of the quadrangle. The plains rise to the south to form the north edge of the Amazonis Planitia and to the southeast toward two major volcanic provinces of Mars, Olympus Mons and Alba Patera. The aureole deposits of these knobby terrain occurs in the southwestern part of the quadrangle and rises toward the Elysium volcanic province that lies 1600 km to the west. Original mapping of this quadrangle was from Mariner 9 pictures. The mapping was...
This map is one in a series of 1:500,000-scale geologic maps initiated by NASA to investigate areas of particular scientific interest on Mars. The north Kasei Valles area merits detailed geologic study because it contains part of a large channel system whose age can be determined relative to geologic units that range in age from early intermediate (Early Hesperian) to the very late (Late Amazonian) periods of Martian history. Also, many geomorphic features in the map area suggest changes in water level and multiple erosional events associated with the Kasei Valles system. Later erosional events are indicative of spring sapping; small-scale, ground-water runoff; and water-mobilized debris flow. Therefore, this large-scale...
The Pompeii quadrangle is in northern Maja Valles region between Lunae Palum to the west and Xanthe Terra to the east. Approximately two-thirds of the surface is a relatively smooth plain, and the other one-third is subdued, cratered, upland plateau. The crater Pompeii is the largest fresh crater in the quadrangle. The major interest in the map area is evidence of the relatively brief, catastrophic Maja outflow and its associated topographic modification of much of the area. The effects of erosion and deposition by the Maja flood are pronounced and are a chief part of the story; therefore, flood-modified terrain is divided in considerable detail. The stratigraphic units associated with the outflow are true rock...
The Purbach quadrangle is in the south central part of the lunar near side and includes the following four distinct topographic geologic provinces: 1) rugged and densely cratered highlands extending north south through the central part of the area locally dissected by large troughs (sculpture) of Imbrium age (Gilbert, 1893; Hartmann, 1963) 2) subdued terrain in the east where both isolated and interconnected topographic lows are partly filled with plains material 3) terra and plains materials of low relief in the southwest which obscure the large ancient crater Deslandres; 4) basalt flows of Mare Numbium which embay and overlap the adjacent terrae along the west central and northwestern parts of the quadrangle.
Mariner 10 data include complete photographic coverage of the quadrangle at a resolution of about 2 km. In addition, twelve stereopairs cover scattered areas in the quadrangle (Davies and others, 1978, p. 114-115); these photographs were used to supplement the geologic interpretation. About 10° of longitude of the H-13 quadrangle (Solitudo Persephones Province) adjacent to the west is included in the map area because not enough Mariner 10 data were acquired of this quadrangle to justify the production of another map.
Incorporated into USGS OpenFile Report #1094, "The Geologic Classification of the Meteorites", these materials were written by Donald Elston and contain figures, photos, and charts to help astronauts (who were not trained geologists) be able to identify and articulately describe the geologic observations they made on the lunar surface.
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