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Cutts, J. A.

Publications and source records attributed to Cutts, J. A..

At least 55 records · Page 3
All sourcesNASA NTRSDOE OSTI
NASA NTRS1976

Planetary imaging - Past, present, and future

Recent exploration of the planets has been highlighted by the development of visual imaging systems carried on board the spacecraft. This paper describes the evolution of planetary camera systems from the earliest reconnaissance flight to Mars in 1965 (Mariner 4) through the planned mission to Jupiter and Saturn in 1977. Advances in telecommunication performance, mission planning and operations, and digital processing of images are also discussed. Science objectives and changes in the imaging systems required to meet these objectives are discussed for the Mariner Mars 1971 (Mariner 9), Mariner Venus-Mercury (Mariner 10), Viking 1975 (Mars Orbiter), and Mariner Jupiter-Saturn 1977 missions. The last section of the paper describes future plans for imaging experiments based on cameras using solid-state sensors, particularly charge-coupled devices.

Masursky, H.↗
NASA NTRS1976

Shield volcanism and lithospheric structure beneath the Tharsis plateau, Mars

The heights of four great shield volcanoes, when interpreted as reflecting the local hydrostatic head on a common source of upwelling magma, provide significant constraints on models of lithospheric structure beneath the Tharsis plateau. If Bouguer gravity anomalies are modeled in terms of a variable thickness crust, and a two-component (crust/mantle) earth-like structure is assumed for the Martian lithosphere, the derived model lithosphere beneath the Tharsis plateau has the following properties: (1) the upper low-density 'crustal' component is thickened beneath the Tharsis plateau; (2) the lower high-density 'mantle' component is thinned beneath the Tharsis plateau; and (3) there is a net gradient on the base of the Martian lithosphere directed downward away from beneath the summit of the Tharsis plateau. A long history of magmatic intrusion is hypothesized to have been the cause of the updoming of the Tharsis plateau and the maintenance of the plateau in a state of only partial compensation.

Blasius, K. R.↗
NASA NTRS1974

Mariner Mars 1971 television picture catalog. Volume 1: Experiment design and picture data

A compilation of Mariner 9 television data is presented for the study of the planet Mars and of its two satellites, Phobos and Deimos. The concept of the basic mission, camera characteristics, and various processing techniques of the raw television data recovered from the spacecraft are discussed. Data are arranged into the following disciplines; (1) mapping and geology, (2) polar studies, (3) geodesy, (4) variable surface features, (5) atmospheric phenomena, and (6) satellites. Reproduction and arrangements of approximately 3000 individual pictures and photomosaics are provided.

Cutts, J. A.↗
NASA NTRS1973

Television experiment

The fixed and variable Martian features investigated by the TV experiment on Mariner 9 are described. Articles are presented concerning the dust storm of October to November over the Southern Hemisphere; global surface geodesy and cartography; geology; and the satellite astronomy.

Briggs, G. A.↗
NASA NTRS1973

Volatiles working group

The physical behavior of water and carbon dioxide on Mars was studied. Topics discussed include: physics of polar frosts, CO2 budget, atmospheric minor constituents, chemical and physical properties of surface materials, layered deposits, and the role of volatiles in the Martian landscape formation.

Cutts, J. A.↗
NASA NTRS1973

Eolian deposits and dunes on Mars

Detailed analysis of the Mariner 9 pictures reveals that eolian activity is not only a superficial effect, but a surface process of profound importance in the geologic evolution of Mars. Moderate- and large-scale topographic features that may be attributed to wind erosion are described and latitudinal variations in crater morphology are interpreted in terms of eolian deposition and erosion in the mid-latitudes of Mars.

Cutts, J. A.↗
NASA NTRS1973

Mariner 9 observations of the surface of Mars in the north polar region

The recession rate of the north polar cap, as monitored by Mariner 9, was not significantly different than has been observed from earth in the past. Thus, the dynamic planet-wide dust storm does not seem to have had a noticeable effect on the thickeness of the CO2 deposit which developed during the standard mission. The dominant role of local topography in controlling the configuration of the retreating cap is confirmed. At narrow-angle resolution the retreating frost has high-lighted topographic detail that may represent Martian polar eolian deposits. At wide angle resolution the topography of the smooth plains, rugged etch pitted terrain, and complex central polar deposits is emphasized by the frost.

Soderblom, L. A.↗
NASA NTRS1973

Wind erosion in the Martian polar regions

Photographic evidence suggests that many topographic features of the polar regions of Mars may have been sculptured by wind action. In the case of the pitted terrain, this is established by relating the orientations of elongate basins and grooves to patterns of albedo markings that are generally accepted to be wind-formed. Small-scale flutes and other textures of laminated terrain recognized outside the perennial ice cap in the south polar region are also attributed to eolian action. Winds flowing off the polar cap and spiraling toward the west seem to be responsible. More speculatively the large-scale circumpolar features which underlie the residual polar caps may be related to wind erosion. Rotational motion localized on circular segments of the perennial frost deposits are proposed as a mechanism.

Cutts, J. A.↗
NASA NTRS1973

Nature and origin of layered deposits of the Martian polar regions

Layered deposits in the Martian polar regions are interpreted as accumulations of dust derived from atmospheric suspensions. Depressed and eroded terrains of the equatorial region are considered to be the principal sources of dust. A depositional model based on polar precipitation of dust predicts the formation of a vast, dome-shaped, featureless plateau underlain by layered deposits and occupying most of the area of annual frost cover. The rates of accumulation of dust and water ice in the polar regions have been estimated on the basis of atmospheric conditions in the present era. The analysis indicates an accumulation time of about 500 x 1 million years for the layered deposits and the presence of significant quantities of water ice in the deposits beneath the perennial cap.

Cutts, J. A.↗
NASA NTRS1973

Eolian deposits and dunes on Mars.

A complex of coalescing ridges and diverse marginal features observed in Mariner 9 pictures of the Hellespontus region of Mars is identified as a dune mass. Many other possible dune features are recognized in midlatitudes and polar latitudes, and regional differences in the appearance of cratered terrains are attributed to modification by dune deposits. The morphology and temporal behavior of some Martian albedo features can be explained by dune-forming saltation processes. Eolian activity seems to be widespread, if not ubiquitous, on Mars and appears to produce major regional variations in the surface environment.

Cutts, J. A.↗
NASA NTRS1973

Mariner 9 observations of the surface of Mars in the north polar region.

During the Mariner 9 extended mission the recession of the north polar ice caps was monitored for 130 days. The edge of the cap displayed a peculiar polygonal outline during most of this period. Regional topographic control is suggested as the most likely cause of the polygonality. Whereas densely cratered terrain dominates the south polar region, moderately cratered plains underlie the polar deposits in the north polar region. The mottled cratered plains have been mantled by light deposits located in annular rings south of 70 N. The erosional boundaries between these deposits and the subjacent cratered plains are gradational, show no local topographic relief, and display a spiral serrated circumpolar pattern suggesting eolian erosion. Smooth plains and 'etch-pitted' plains underlie the central polar layered deposits in both polar regions. In addition, these plains have one other morphological variant in the north. Here they display a pattern of very coherent ripple-like waveforms varying in wavelength from several hundred meters to a few kilometers.

Soderblom, L. A.↗
NASA NTRS1973

Wind erosion in the Martian polar regions.

Wind erosion may have played a dominant role in sculpturing the terrains of the polar regions of Mars. Many topographic features of the pitted terrain and the laminated terrain are consistently aligned with wind directions inferred from albedo markings. Cold air outflow from the polar cap veering to the west as a result of the coriolis force may account for the observed alignments. The remarkable pseudocircular and spiral features that underlie the residual frost caps in both polar regions may have been formed by the more complex circulation patterns of the inner polar zone.

Cutts, J. A.↗
NASA NTRS1973

Nature and origin of layered deposits of the Martian polar regions.

Layered deposits in the polar regions of Mars may be formed from fine dust ultimately derived from the canyons and other eroded terrains of the equatorial regions. An analysis of dust deposition in the area of annual frost cover predicts the formation of vast featureless domed plateaus underlaid by layered deposits of dust. Television observations suggest that these plateaus once existed, but they have now been dissected and stripped from most of the area of annual frost cover. A possible explanation is that a major secular change has occurred in the erosional environment of the Martian polar regions. Estimates of depositional rates of dust under current atmospheric conditions place the time span represented by the accumulation of layered deposits at about 500 m.y. Because of erosion, the present surface appears very young and lacks any impact craters. The present rate of water ice accumulation in the area of perennial frost is comparable to that of dust, and thus it is suggested that large quantities of water ice may be trapped with dust beneath the perennial frost caps.

Cutts, J. A.↗
NASA NTRS1973

Mariner 9 - Image processing and products.

The purpose of this paper is to describe the system for the display, processing, and production of image-data products created to support the Mariner 9 Television Experiment. Of necessity, the system was large in order to respond to the needs of a large team of scientists with a broad scope of experimental objectives. The desire to generate processed data products as rapidly as possible, coupled with the complexities introduced by the nature of the vidicon camera, greatly increased the scale of the ground-image processing effort. This paper describes the systems that carried out the processes and delivered the products necessary for real-time and near-real-time analyses. References are made to the computer algorithms used for the different levels of decalibration and analysis.

Levinthal, E. C.↗
NASA NTRS1973

Exploration of Mars by Mariner 9 - Television sensors and image processing.

Two cameras equipped with selenium sulfur slow scan vidicons were used in the orbital reconnaissance of Mars by the U.S. Spacecraft Mariner 9 and the performance characteristics of these devices are presented. Digital image processing techniques have been widely applied in the analysis of images of Mars and its satellites. Photometric and geometric distortion corrections, image detail enhancement and transformation to standard map projection have been routinely employed. More specializing applications included picture differencing, limb profiling, solar lighting corrections, noise removal, line plots and computer mosaics. Information on enhancements as well as important picture geometric information was stored in a master library. Display of the library data in graphic or numerical form was accomplished by a data management computer program.

Cutts, J. A.↗
NASA NTRS1972

Preliminary Mariner 9 report on the geology of Mars.

Mariner 9 results indicate that Mars is geologically far more heterogeneous than previously suspected from earlier flyby missions; the surface has been shaped by volcanic, tectonic, erosional, and depositional activity. The equatorial region between 30 deg N and 30 deg S latitude is depicted in four geologic sketch maps, and seventeen geologic units are defined on the basis of their textural characteristics. The maps and the brief descriptions of geological units portrayed are followed by a series of more interpretive discussions dealing with topical problems and a summary geologic history. Topics covered include cratering, circular basins, volcanism, canyons, chaotic terrain, channels, and eolian activity.

Mccauley, J. F.↗
NASA NTRS1972

Geological framework of the south polar region of Mars.

The first 4 months of Mariner 9 photography of the south polar region are discussed. Three major geological units have been recognized, separated by erosional unconformities. From oldest to youngest they are: cratered terrain, pitted plains, and laminated terrain. The latter unit is unique in occurrence to the polar region, volatiles are probably involved in its origin, and may still be present within the laminated terrain as layered ice. The residual south polar cap has been observed to survive the disappearance of the thin annual CO2 frost deposit and to last virtually unchanged in outline through the southern summer. That exposed deposit is inferred to be composed of water-ice. The residual cap appears to lie at the apex of an unusual quasi-circular structure composed of laminated terrain; a similar structure also appears to exist near the north pole.

Murray, B. C.↗