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Wildey, R. L.

Publications and source records attributed to Wildey, R. L..

At least 19 records
All sourcesNASA NTRSDOE OSTI
NASA NTRS1986

Radarclinometry for the Venus radar mapper

Already van Diggelen (1951) made use of the photometric function of a surface for the purpose of translating image variegation into slope and relief information, while the development of a method for producing a topographic map from a photometric image begins with Rindfleisch (1966). The term 'photoclinometry' was invented for the involved process. The present study is concerned with the adaptation of photoclinometry to radar imagery. The radar image as a candidate for photoclinometry offers both advantages and disadvantages when compared to ordinary optical images. The simplicity of the photometric function is the most obvious advantage. Attention is given to radiative transfer, the employment of differential geometry, and aspects of calibration.

Wildey, R. L.↗
NASA NTRS1985

The determination of physical and dynamical parameters of Pluto/Charon and binary asteroids by least-square formation of a matched filter for a time series of images. I - The operational theory

A theory is derived for the determination of the masses, radii, and orbital elements of the Pluto/Charon, or similar, system based on the prediction of an image distribution over space and time and its comparison with observation. The comparison may be ultimately through the theory of least squares or the application of a matched filter to the observations as a three-dimensional signal stream at an initial or intermediate state. The theory is an approximation correct to fifth order in the diameters of celestial bodies. The theory of astronomical seeing that is used is based on Kolmogorov turbulence in the long-exposure limit. The images must be photometric. Linear tracking errors that can be removed are preferable to either automatic or manual guiding, in the collection of candidate observations.

Wildey, R. L.↗
NASA NTRS1985

Progress in Planetary Radarclinometry

Efforts have continued to improve radarclinometry in spite of the fact that the theory and algorithms still predate the development of the radiometrically calibrated radar upon which they must depend in order to achieve metric precision. Such efforts help to insure the availability of the technique for data returned by the Venus Radar Mapper. Even now, compensation for layover and production of synthesized stereo enhance geologic interpretability of radar images. The theory of radarclinometry utilizes a knowledge of the relation between pixel DN value and terrain surface orientation to produce a topographic map. The process may be conceived in terms of a surface integral which develops away from a topographic profile as available ground truth. Alternatively, in consideration of the unavailability of ground truth in extraterrestrial applications, radarclinometry may develop as a line integral developing from a single point, providing reasonable assumptions about the mathematical nature of local curvature.

Wildey, R. L.↗
NASA NTRS1978

The moon in Heiligenschein

An analysis of 25 photometric digital images of the moon has been carried out to obtain a single image in a new mapping parameter, the Heiligenschein exponent. The data necessarily represent a range of lunar phases, but all are within 10 hours of full moon. The new parameter characterizes the rate at which lunar features brighten as their local phase angles approach zero. Although considerable contrast is present in this parameter, there is only a small corelation with normal albedo. In particular, the large albedo difference between maria and highlands is not simply reflected in Heiligenschein differences, which are larger within each category of terrain than the difference between the Heiligenschein averages of each. A correlation with age may be present in both the maria and the highlands, but its determination will require separation into distinct geochemical provinces.

Wildey, R. L.↗
NASA NTRS1978

Correlation of chemistry with normal albedo in the Crisium region

The region in the vicinity of the Luna 24 handling site (40-70 deg E; 0-20 deg N) is studied by means of the Apollo orbital fluorescent X-ray Al/Si and Mg/Al data and earth-based normal albedo measurements. By means of unsupervised non-parametric cluster analysis this region is divided into eight surface units. One of these units centered in the Proclus region deviates from the usual trend of increasing normal albedo with increasing Al/Si values and decreasing Mg/Al values

Bielefeld, M. J.↗
NASA NTRS1975

Generalized photoclinometry for Mariner 9

A theory is developed for the photoclinometric determination of topography when the photometric function of a planetary surface is not restricted beyond the expectation that it is a function of phase angle, angle of incidence, and angle of emergence. Several versions of such an operational theory are presented together with several approaches to the numerical analysis. Reasons for the differences in numerical techniques are discussed. A preliminary result is considered which has been produced for an early Mariner 9 frame wherein the dust-laden atmosphere seems to exhibit standing-wave patterns. It is shown that if the assumption of homologous departures from plane-parallel atmospheric configuration is valid, the photoclinometry implies that laminar flow lines in the optically observable dust layer undergo a near-sinusoidal rise and fall of about 40 to 50 meters.

Wildey, R. L.↗
NASA NTRS1973

Theoretical autophotogrammetry. I - The method of the photometric potential

The present work presents preliminary efforts at a mathematical formulation of a photogrammetric method suitable for computerized processing. A theory is derived for the extraction of surface topography from stereometric pairs of photographs. The theory can be applied to either convergent or near-orthographic-projection stereo. Scene brightness is treated as a scalar function defined on a general surface embedded in ordinary three-dimensional space (the actual topography). Correspondence of points is based on adjustments leading to photometric equivalence, while the adjustments are based on the local value of the photometric gradient.

Wildey, R. L.↗
NASA NTRS1972

The Martian atmosphere - Mariner 9 television experiment progress report.

Atmospheric phenomena appearing in the Mariner 9 television pictures are discussed in detail. The surface of the planet was heavily obscured by a global dust storm during the first month in orbit. Brightness data during this period can be fitted by a semi-infinite scattering and absorbing atmosphere model with a single-scattering albedo in the range 0.70-0.85. This low value suggests that the mean radius of the particles responsible for the obscuration was at least 10 microns. By the end of the second month, this dust storm had largely dissipated, leaving a residual optical depth of about 0.1. Much of the region north of 45 deg N was covered by variable clouds comprising the north polar hood.

Leovy, C. B.↗
NASA NTRS1972

Mariner 9 television reconnaissance of Mars and its satellites - Preliminary results.

At orbit insertion, the Martian surface was largely obscured by a dust haze with an extinction optical depth that ranged from near unity in the south polar region to probably greater than two over most of the planet. The only features clearly visible were the south polar cap, one dark spot in Nix Olympica, and three dark spots in the Tharsis region. During the third week, the atmosphere began to clear and surface visibility improved, but contrasts remained a fraction of their normal value. Each of the dark spots that apparently protrude through most of the dust-filled atmosphere has a crater or crater complex in its center. The craters apparently were formed by subsidence and resemble terrestrial calderas.

Masursky, H.↗
NASA NTRS1972

Regional variations in the magnitude of heiligenschein and causal connections, part O

A preliminary quantitative analysis was conducted of four frames exposed by the Apollo 15 metric camera. Two of the frames show the zero-phase surge on maria and the other two show the surge on terrae. It was found that the curves resulting from brightness plotted as a function of phase angle, differ markedly according to which terrain type is involved. The magnitude of the heiligenschein was found to be significantly greater for the maria than for the terrae.

Wildey, R. L.↗
NASA NTRS1972

Physical and geological aspects of heiligenschein measurements, part Y

A preliminary attempt was made to evaluate the geological significance of the dispersion in the heiligenschein index. Heiligenschein coordinates were plotted on the 1:5,000,000 geologic map of the near side of the moon. The purpose was to evaluate the specific geologic unit involved in the case of each heiligenschein display. Tentative results that list the mean heiligenschein index and the rms deviation for each geologic map unit are given.

Wildey, R. L.↗