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Geology topics

Richard J. Pike

Publications and source records attributed to Richard J. Pike.

28 records · Page 2Linked to original sources
USGS1978

Lunar landscape morphometry

This report outlines some general methods for analyzing the geometry of planetary topography and illustrates them with results obtained for the Moon. Its contents apply to selection of landing sites for spacecraft, planning traverses for vehicles, and to other aspects of planetary exploration that involve numerical expression of topographic form primarily for engineering purposes. The report is divided into three separate sections. Part I treats descriptive and predictive techniques for terrain slope. Part II describes the analysis of fine-scale surface roughness for the NASA Lunar Roving Vehicle, which was first deployed on Apollo mission 15 in the Hadley Rille area of the Moon. Part III applies the method of numerical taxonomy to multivariate characterization of lunar terrain and geologic map units. Although the findings described here are for the Moon only, the approaches and techniques could be used to solve terrain-related problems on any of the terrestrial planets. The author hopes that this study will stimulate further research in both terrestrial and extraterrestrial landscape morphometry.

Open-File Report↗
USGS1978

Terrain-analysis procedures for modeling radar backscatter

The collection and analysis of detailed information on the surface of natural terrain are important aspects of radar-backscattering modeling. Radar is especially sensitive to surface-relief changes in the millimeter- to-decimeter scale four conventional K-band (~1-cm wavelength) to L-band (~25-cm wavelength) radar systems. Surface roughness statistics that characterize these changes in detail have been generated by a comprehensive set of seven programmed calculations for radar-backscatter modeling from sets of field measurements. The seven programs are 1) formatting of data in readable form for subsequent topographic analysis program; 2) relief analysis; 3) power spectral analysis; 4) power spectrum plots; 5) slope angle between slope reversals; 6) slope angle against slope interval plots; and 7) base length slope angle and curvature. This complete Fortran IV software package, 'Terrain Analysis', is here presented for the first time. It was originally developed a decade ago for investigations of lunar morphology and surface trafficability for the Apollo Lunar Roving Vehicle.

Open-File Report↗
USGS1973

Crater studies: Part A: lunar crater morphometry

Morphometry, the quantitative study of shape, complements the visual observation and photointerpretation in analyzing the most outstanding landforms of the Moon, its craters (refs. 32-1 and 32-2). All three of these interpretative tools, which were developed throughout the long history of telescopic lunar study preceding the Apollo Program, will continue to be applicable to crater analysis until detailed field work becomes possible. Although no large (>17.5 km diameter) craters were examined in situ on any of the Apollo landings, the photographs acquired from the command modules will markedly strengthen results of less direct investigations of the craters. For morphometry, the most useful materials are the orbital metric and panoramic photographs from the final three Apollo missions. These photographs permit preparation of contour maps, topographic profiles, and other numerical data that accurately portray for the first time the surface geometry of lunar craters of all sizes. Interpretations of craters no longer need be compromised by inadequate topographic data. In the pre-Apollo era, hypotheses for the genesis of lunar craters usually were constructed without any numerical descriptive data. Such speculations will have little credibility unless supported by accurate, quantitative data, especially those generated from Apollo orbital photographs. This paper presents a general study of the surface geometry of 25 far-side craters and a more detailed study of rim-crest evenness for 15 near-side and far-side craters. Analysis of this preliminary sample of Apollo 15 and 17 data, which includes craters between 1.5 and 275 km in diameter, suggests that most genetic interpretations of craters made from pre-Apollo topographic measurements may require no drastic revision. All measurements were made from topographic profiles generated on a stereoplotter at the Photogrammetric Unit of the U.S. Geological Survey, Center of Astrogeology, Flagstaff, Arizona.

Book chapter↗
USGS1972

Photogeology: Part L: crater morphometry

Morphometric analysis of lunar craters (ref. 29-75) complements the more traditional photointerpretive study of crater morphology. These two indirect approaches to the scientific investigation of lunar craters continue to be productive because the preferred alternative method, direct field examination of specific large craters, is not being undertaken in the current series of manned lunar landings and will not be implemented for some time. Metric camera photography returned from the Apollo flights is essential to the continued study of lunar crater geometry. The material provides raw data of a quality far superior to and more uniform than comparable data available from Lunar Orbiter or Earth-based sources.

Book chapter↗
USGS1971

Elevation-relief ratio, hypsometric integral, and geomorphic area-altitude analysis

Mathematical proof establishes identity of hypsometric integral and elevation-relief ratio, two quantitative topographic descriptors developed independently of one another for entirely different purposes. Operationally, values of both measures are in excellent agreement for arbitrarily bounded topographic samples, as well as for low-order fluvial watersheds. By using a point-sampling technique rather than planimetry, elevation-relief ratio (defined as mean elevation minus minimum elevation divided by relief) is calculated manually in about a third of the time required for the hypsometric integral.

Bulletin of the Geological Society of America↗