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Geology topics

T.A. Mutch

Publications and source records attributed to T.A. Mutch.

8 recordsLinked to original sources
USGS1979

Geologic map of the Memnonia Quadrangle of Mars

The Memnonia quadrangle lies astride the boundary between heavily cratered and sparsely crater ed 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 slopes of the Tharsis Montes, which con tinue to rise in elevation eastward in t o the adjacent Pheo nicis Lacus and Tharsis quadrangle. There is little correlation between terrain types and elevation within the Mamnonia quadrangle. In particular , the boundary between cratered terrain and plains for the most part is not marked by any prominent change in elevation .

IMAP↗
USGS1976

The surface of Mars: The view from the Viking 1 lander

The first photographs ever returned from the surface of Mars were obtained by two facsimile cameras aboard the Viking 1 lander, including black-and-white and color, 0.12° and 0.04° resolution, and monoscopic and stereoscopic images. The surface, on the western slopes of Chryse Planitia, is a boulder-strewn deeply reddish desert, with distant eminences—some of which may be the rims of impact craters—surmounted by a pink sky. Both impact and aeolian processes are evident. After dissipation of a small dust cloud stirred by the landing maneuvers, no subsequent signs of movement were detected on the landscape, and nothing has been observed that is indicative of macroscopic biology at this time and place.

Science↗
USGS1976

Fine particles on Mars: Observations with the Viking 1 lander cameras

Drifts of fine-grained sediment are present in the vicinity of the Viking 1 lander. Many drifts occur in the lees of large boulders. Morphologic analysis indicates that the last dynamic event was one of general deflation for at least some drifts. Particle cohesion implies that there is a distinct small-particle upturn in the threshold velocity-particle size curve; the apparent absence of the most easily moved particles (150 micrometers in diameter) may be due to their preferential transport to other regions or their preferential collisional destruction. A twilight rescan with lander cameras indicates a substantial amount of red dust with mean radius on the order of 1 micrometer in the atmosphere.

Science↗
USGS1973

Preliminary geologic map of the Memnonia quadrangle of Mars, Viking Mars 1975 landing site

This mosaic is made with computer-enhanced, unrectified Mariner 9 pictures provided by The Jet Propulsion Laboratory Mission and Test Video System (MTVS). The Vertical Automatic Gain Control (Vert. AGC) version is used. The pictures were scaled for a "best fit" by the U.S. Geological Survey using spacecraft tracking data. Discrepancies between image positions are as large as one degree in latitude and longitude.

Open-File Report↗
USGS1972

Imaging experiment: The Viking Lander

The Viking Lander Imaging System will consist of two identical facsimile cameras. Each camera has a high-resolution mode with an instantaneous field of view of 0.04°, and survey and color modes with instantaneous fields of view of 0.12°. Cameras are positioned one meter apart to provide stereoscopic coverage of the near-field. The Imaging Experiment will provide important information about the morphology, composition, and origin of the Martian surface and atmospheric features. In addition, lander pictures will provide supporting information for other experiments in biology, organic chemistry, meteorology, and physical properties.

Icarus↗
USGS1972

Geologic map of the Hommel quadrangle of the Moon

The Hommel quadrangle is in the southeas t highlands of the earthside hemisphere of the Moon. The major geologic units are smooth and ridged terra materials, plains-forming materials, and crater materials. Mare material is absent. In the absence of extensive stratigraphic datum horizons, the geologic units were tentatively correlated with type areas of the lunar geologic system (Shoemaker and Hackman, 1962; Wilhelms , 1970) by means of a graded sequence of crater morphologies.

IMAP↗
USGS1967

Preliminary geologic map of Ellipse III-9-5 and vicinity

Ellipse III-9-5 is in a level area between Mare Cognitum and Oceanus Procellarum, approximately 125 km southeast of the crater Lansberg. Mare material within the map area is covered with a greater number of subdued craters than typical smooth mare.

Open-File Report↗