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The Valles Marineris region lies east of Tharsis Montes (which extend from lat 12 degrees to 16 degrees., long 101 degrees to 125 degrees). 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...

Olympus Mons is the largest known volcanic construct in the Solar System; it is more than 600 km across and more than 27 km above datum. The volcano and the great scarp that bounds it have been the subject of much scientific controversy. Although it has been possible to generate an empirical model that closely resembles Olympus Mons, the dynamics of scarp formation are still unproven...

This map is one in a series of 1:500,000-scale geologic maps initiated by the National Aeronautic 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...

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 north Kasei Valles area (fig. 1) 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

The region centered at Elysium Mons contains that second largest volcanic complex on Mars, surpassed in size by only the Tharsis complex. The Elysium region also has been a center of tectonic, fluvial, and mass-wasting activity. After degradation of ancient cratered terrain within the northern lowlands, volcanic rocks erupted from Elysium Mons, Hectas Tholus, and Albor Tholus in Elysium...

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

Mangala Valles are a system of outflow channels cut into Terra Sirenum that appear to originate from a fracture of Memnonia Fossae radial to the Tharsis volcanic center (about 1,800 km to the east).

The map area is in the Mangala-Memnonia region (fig. 1), which contains remarkably diverse geologic features and terrain types. Studies of the Mariner 9 images revealed the wide range of ages of the major rock units in this region; age assignments were based on the density of impact craters preserved on the various surfaces (Mutch and others, 1976, p. 56-60; Scott and Carr, 1978; Mutch...

The geology for this map was compiled using Viking Orbiter images on 1:500,000- scale photomosaics of the Mars Transverse Mercator quadrangles -40262, -40267, and -40272. This map represents a detailed extension of regional geologic mapping of the east Hellas rim (Crown and others 1990, 1992) and is published at 1:1,000,000 scale. The map area is on the east rim of one of the largest...

The surface of the moon is heterogeneous. The differences from area to area of characteristic topographic forms and of physical properties such as albedo (reflectivity under full-Moon illumination) indicate that the materials underlying the surface vary from one area to another and that different processes have operated in the development of the surface. In lunar geologic mapping, areas...

The area shown on this map includes layered polar deposits and residual polar ice, as well as some exposures of older terrain. Howard and others (1982) noted that an area (at lat 84.8 S., long 356 W.) near a 23-km diameter impact crater (Plaut and others, 1988) appears to have undergone recent deposition, as evidenced by the partial burial of secondary craters. Herkenhoff and Murray...

The polar deposits on Mars are of great interest because they probably record martian climate variations (Thomas and others, 1992). The area shown on this map includes polar layered deposits with distinct low-albedo features and a sharp boundary between the layered deposits and the moderately cratered unit that forms the floor of Chasma Australe. Detailed mapping of this quadrangle was...