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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.
This 1:250,000-scale geologic map is one of a series prepared largely from photographs transmitted by Ranger IX (reproduced in a report by Jet Propulsion Lab., 1966). It depicts the geology of the crater Alphonsus (in which Ranger IX impacted) and environs. The primary objective of the mapping was to apply extent lunar mapping techniques used on relatively small scale telescopic photographs to the larger scale Ranger photographs, in preparation for extensive analysis of lunar orbiter photography in support of the apollo program. An additional objective was to shed more light on the formation of Alphonsus and its associated features. The map outlines rock units that are inferred from surface features and characteristics,...
The Cassini quadrangle is in the north-central part of the nearside lunar disk and includes most of the northeast quadrant of Mare Imbrium. Four principle classes of geologic units can be distinguished: (1) material of three rugged arcuate mountain ranges circumferential to the imbrium basin; (2) terra materials superposed on these ranges; (3) mare materials; and (4) crater materials.
This map is one of a series showing the geology of areas of special scientific interest - areas considered as candidate sites for Apollo landings. Many of these sites were dropped from the list of candidates owing to operational constraints and curtailment of the Apollo program, together with priority judgments of relative scientific merit. The preliminary work on these areas has been refined, and the maps are being published with a view toward their use in possible future lunar exploration programs, either manned or unmanned. The mapping was done mostly with Lunar Orbiter data, using the methods described by Wilhelms (1970) and Trask (1969).
The surface of the moon is heterogenous. Similar surface materials are grouped into map units by means of telescope observations, study of lunar photographs, and photometric measurements. Each map unit has lateral continuity and limited range of physiographic characteristics and optical properties (mainly albedo, the reflectivity under full moon illumination). Such units are equivalent to the rock stratigraphic formations of terrestrial geology. By application of the principles of superposition and intersection, these formations have been arranged in order of relative age and grouped into time stratigraphic units. Following terrestrial convention, the major time-stratigraphic units are designated systems; corresponding...
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...
Published geologic maps of the south polar region of Mars, made using either Mariner 9 (Condit and Soderblom, 1978) or Viking Orbiter (Tanaka and Scott, 1987) images, identified only layered deposits and polar ice within this map area. Layered deposits probably underlie all of the other units shown on this map. The residual polar ice cap, partial frost cover, and two low-albedo units are also mapped here. These units were first recognized and mapped by Herkenhoff and Murray (1990a) at 1:2,000,000 scale using color mosaic of Viking orbiter images. This mosaic and an additional Viking color mosaic were used to confirm the identification of the five mapped color/albedo units. The colors and albedos of these units are...
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...
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