SEARCH · Search USGS
Search indexed USGS publications on groundwater, aquifers, geologic maps, mineral resources and earthquakes. Explore source records by subject and place.
Quote a phrase for an exact phrase match. Source license links do not imply unrestricted reuse.
The pattern of rock units in the geologic map of the New Windsor quadrangle has been affected by three distinguishable generations of folds; following the usage of Tobisch and Fleuty (1969) and Higgins (1973), the fold generations are named for localities where they are well displayed.
Geologic units of the martian surface are subdivided on the basis of surface morphology, albedo, and crater distribution and are placed in a stratigraphic sequence following principles of superposition, crosscutting relations, and, to a degree, crater density. The Casius quadrangle (30˚ N to 65˚ N lat; 240˚ W to 300˚ W long) is one of the northern tier of Lambert conformal sheets of the Mars Atlas. It consists of four distinctive physiographic regions: 1) part of the northern cratered plains which forms an incomplete annulus around the north polar region, 2) smooth lowland plains of Utopia Planitia across the central and southeastern part of the map, 3) mountainous terrain, in the Nilosyrtis Mensae region south of the lowland plains, consisting of distinct mountains with hummocky surfaces, and 4) cratered plateau in the southwest part of the map, forming the northern part of the large complex cratered region in the mid-latitudes of Mars. In the Casius quadrangle, the cratered plateau is broken by a set of linear to curved parallel-sided canyons on its northern margin.
Explore the source record for details and available documents.
Explore the source record for details and available documents.
Explore the source record for details and available documents.
Explore the source record for details and available documents.
No abstract available.
Explore the source record for details and available documents.
Explore the source record for details and available documents.
Explore the source record for details and available documents.
This map is one of a series of geologic maps t hat will cover the entire Moon at a scale of 1:5,000,000. The geology of the central far side is compiled largely from NASA Lunar Orbiter and Apollo photographs and Soviet Zond photographs; the discussion and interpretation of geologic units incorporate the geochemical and geophysical data obtained from orbiting s p acecraft. Geologic units are based on the stratigraphic framework established by Shoemaker and Hackman (1962) as subsequently revised (summarized by McCauly , 19 67 ; Wilhelms , 1970; Mutch , 1972; Stuart-Alexander and Wilhelms , 1975). Description of map units is brief because they largely follow units described on the nearside 1:5,000,000 map of Wilhelms and McCauley (1971). The reader unfamiliar with lunar maps, mapping principles, and terminology is referred to that map. Only new units and features or units whose origins are still much in doubt are discussed here.
The Amazonis quadrangle lies within the northern sparsely cratered hemisphere of Mars ( Carr and others, 19 73) The dominant structural ad physiographic features of the quadrangle are low feature - less 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, a n d in a area of rough knobby terrain along the west edge of the quadrangle. The central plains descend northward into the circumpolar lowlands (Arcadia Plan itia, Vastitas Borealis) and rise southward where they are bounded by the cratered terrains of the equatorial region of Mars.
Explore the source record for details and available documents.
Explore the source record for details and available documents.
Explore the source record for details and available documents.
Explore the source record for details and available documents.
Explore the source record for details and available documents.