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Green, R. R.

Publications and source records attributed to Green, R. R..

At least 19 records
All sourcesNASA NTRSDOE OSTI
NASA NTRS1985

Fast Dual Analog-to-Digital Converter

Unit delivers blocks of quadrature data to computer memory. Contains 105 integrated circuit packages in 19 by 3 1/2 inch (48.26 by 8.39 cm) rack mounted drawer with internal force air blower. Intended for synchronous sampling of quadrature pairs of data, samples with minimal skew (about 10 nanoseconds) using video-type high-speed sampling technology. Unit equipped for computer controlled self-testing. Originally developed for planetary radar data-acquisition system.

Wallis, D. E.↗
NASA NTRS1981

In situ data analysis on high altitude balloons using microprocessors

It is pointed out that systems currently in use permit an uplink data rate from scientific balloons to satellites of only 100 bit/min. On-board microprocessors, which are able to condense data, can address this problem. An experiment is described that demonstrates the capabilities of inflight data processing by an on-board computer for electric field experiments. It was possible to reduce the data rate by two orders of magnitude with no diminution of data quality.

Schroeder, K. R.↗
NASA NTRS1980

Images of Venus by three-station radar interferometry - 1977 results

During the 1977 inferior conjunction of Venus, radar observations were made using three receiving stations as a multiple interferometer. Maps of surface reflectivity and altimetry were prepared from these observations. The new altimetry maps show considerable improvement in relation to many of the earlier maps made using the two-station interferometer. In particular, there are consistent and explainable correlations between the altimetry and reflectivity maps that did not always exist in the past. The highest-resolution maps (about 8 km) show three isolated mountains having altitudes of approximately 2 km above their environs, a pair of ridges separated by approximately 100 km and extending 800 km, and a few anomalous reflectivity features for which little or no altitude change is observed. Other maps at slightly lower resolution show a bright irregular ringed crater, a few large low-reflectivity regions, a shallow crater 150 km in diameter, a gently sloping mountain, and a short ridge running north-south. Many of the later features have been seen in earlier radar maps and should be useful in refining the spin axis and further characterizing the regolith of certain areas of Venus.

Jurgens, R. F.↗
NASA NTRS1980

Ganymede - Radar surface characteristics

Radar observations of Ganymede at X band show that the surface is unusually bright and has unusual polarization properties. A model of the surface based on large numbers of random ice facets (hence vacuum-ice interfaces) is able to account for these characteristics.

Goldstein, R. M.↗
NASA NTRS1979

Radar observations of asteroid 1 Ceres

Radar observations of asteroid 1 Ceres were made at a 12.6-cm wavelength from the Arecibo Observatory in March/April 1977. The measurements, made with a received circular polarization orthogonal to that transmitted, yield a radar cross section of (0.04 + or- 0.01) piR-squared, for R = 510 km. The corresponding radar reflectivity is less than that measured for any other celestial body. Within the accuracy of measurement, no significant variation of cross section with rotational phase is apparent. The shape of the power spectrum suggests that Ceres is rougher at the scale of the observing wavelength than the moon and inner planets, but smoother than the outer three Galilean satellites.

Ostro, S. J.↗
NASA NTRS1978

Venus radar brightness and altitude images

Seven radar-brightness and altitude images are presented. They are each of a small circular region within the equatorial belt of Venus. Resolution is, typically, 10 by 10 km; altitude contour spacing is 500 m. In addition, an image of the large rough feature, beta, is presented with 25 by 25 km resolution.

Goldstein, R. M.↗
NASA NTRS1978

Radar studies of the Martian surface at centimeter wavelengths - The 1975 opposition

The Goldstone radar system was operated at wavelengths of 3.5 and 12.6 cm to probe the Martian surface during the 1975 opposition. Regions studied in detail by range-Doppler techniques are Syrtis Major, Sinus Meridiani, and the crater Schiaparelli. Average rms slopes of 1.6 and 1.1 deg were measured in Syrtis Major at 3.5 and 12.6 cm, respectively, while the average reflectivity was about 0.064 at both wavelengths. No wavelength dependence of surface roughness was seen in Sinus Meridiani, where rms surface slopes averaged 1.8 deg and the reflectivity was about 0.08. The regions around Schiaparelli were probed at a 12.6-cm wavelength. The echo from the bottom of the crater was undetectable. Operating at 3.5 cm during May and June of 1976, 149 CW echo spectra were obtained near latitude 18 deg, sampling most longitudes including the early Viking landing sites. The average total radar cross section is 4.8% of the geometrical cross section. The diffuse component was estimated to be 1.9%, leaving 2.9% to the average quasi-specular component. The average rms slope is 4.1 deg.

Downs, G. S.↗
NASA NTRS1977

The rings of Saturn - Two-frequency radar observations

Results are reported for a two-frequency dual-polarization radar-echo study of Saturn's rings which involved monostatic operation at a wavelength of 3.5 cm and bistatic operation at 12.6 cm. The radar observations show that the rings effectively depolarize linearly and circularly polarized incident waves at the two wavelengths; that the ring particles are unusually efficient radar reflectors, yielding approximately the same high total cross section at both wavelengths; and that there is an apparent excess of power at the 'central' Doppler shifts when compared with homogeneous scattering models based on the optically observed ring distributions. Several possible explanations for these three radar properties are considered. It is found that a model which hypothesizes a thick cloud of irregular water-ice chunks a few centimeters or larger in radius and a model which postulates a monolayer of multimeter-sized water-frost-coated metallic chunks both seem capable of explaining the first two radar properties. But no consistent explanation is found for the excess low-frequency spectral power.

Goldstein, R. M.↗
NASA NTRS1976

A radar study of the backup Martian landing sites

The Goldstone radar system at DSS 14 was used to probe the Martian surface at 8495 MHz in a narrow strip between -6 deg and -2 deg latitude. The Viking C landing sites lie in this strip, and their altitudes, rms surface slope, and reflectivity are presented.

Downs, G. S.↗
NASA NTRS1976

Venus radar images

The paper presents a set of seven radar brightness images and the corresponding altitude contours of small portions (circular regions of 1500-km diameter) of the Venus surface located at the center of the disk taken in the winter of 1973-1974. The regions imaged are arranged in an equatorial belt on the one face of Venus which is always seen on the occasions of closest approach to earth. A real resolution for the images is, typically, 100 x 10 km, while altitude resolution is 500 m.

Goldstein, R. M.↗
NASA NTRS1976

Radar characteristics of Viking 1 landing sites

Radar observations of Mars at centimeter wavelengths in May, June, and July 1976 provided estimates of surface roughness and reflectivity in three potential landing areas for Viking 1. Surface roughness is characterized by the distribution of surface landing slopes or tilts on lateral scales of the order of 1 to 10 meters; measurements of surface reflectivity are indicators of bulk surface density in the uppermost few centimeters. By these measures, the landing site at 47.5 deg W, 22.4 deg N is rougher than the Martian average, although it may be near the average for elevations accessible to Viking, and is estimated to be near the Mars average in reflectivity. The site at the center of Chryse Planitia, 43.5 deg W, 23.4 deg N, may be an area of anomalous radar characteristics, indicative of extreme, small-scale roughness, very low surface density, or a combination of these two characteristics. Observations of the original Chryse site at 34 deg W, 19.5 deg N indicate that that area is at least twice as rough as the Mars average.

Tyler, G. L.↗
NASA NTRS1975

Radar measurements of Martian topography and surface properties - The 1971 and 1973 oppositions

The Goldstone radar system was used at a wavelength of 12.6 cm to probe the Martian surface during the 1973 opposition. Measurements of range and reflected power were made at least weekly between July 12 and November 24. Surface cells isolated by the radar system were 8 km E-W by 110 km N-S. Altitudes were calculated from signal time delays measured relative to a triaxial ellipsoid and were combined with altitudes measured during the 1971 opposition. Contours of constant altitude were calculated at 200 m intervals between latitudes -14 and -22 deg. These contours are presented in conjunction with Mars charts derived from Mariner 9 television pictures. Reflected power was measured at angles of incidence between -5 and +5 deg. These measurements were combined with those obtained during the 1971 opposition.

Downs, G. S.↗
NASA NTRS1974

A radar brightness and altitude image of a portion of Venus

High-resolution radar data, taken from over the 1500-km circular area that was at the center of the planetary disk on June 20, 1972, show that this part of Venus is nearly flat and cratered. The largest crater is 160 km across, but only about 500 m deep. The smallest craters that can be resolved are about 35 km across.

Rumsey, H. C.↗
NASA NTRS1973

Method and apparatus for a single channel digital communications system

A method and apparatus are described for synchronizing a received PCM communications signal without requiring a separate synchronizing channel. The technique provides digital correlation of the received signal with a reference signal, first with its unmodulated subcarrier and then with a bit sync code modulated subcarrier, where the code sequence length is equal in duration to each data bit.

Couvillon, L. A., Jr.↗
NASA NTRS1973

Single-channel digital command-detection system

System, fabricated of highly-reliable digital logic elements, operates on binary pulse-code-modulated signals and derives internal synchronization from data signal. All-digital implementation of detector develops synchronization from data signal by computer cross-correlation of command modulation signal with its expected forms in sequence and adjusts detector phases in accordance with correlation peaks.

Carl, C. C.↗
NASA NTRS1973

Martian topography and surface properties as seen by radar - The 1971 opposition.

Taking advantage of the favorable opposition of 1971, the Goldstone radar system, operating at 2388 MHz, was used to scan the Martian surface. Measurements of altitude and reflected power were taken approximately every 3 days. Each measurement represents an area 8 km E-W by 80 km N-S, the highest resolution attained to date. Altitude measurements obtained on different observing days were combined to produce altitude profiles for three complete rotations, each at different latitudes. Large-scale variations in altitudes cover a range of 14 km. Altitude changes of 5 in 30 km of longitude were observed. The altitude profiles show the heavy cratering of the surface, and several large craters (50-100 km) 1-2 km deep are easily seen.

Downs, G. S.↗
NASA NTRS1971

Mars radar observations - A preliminary report.

Radar observations of a narrow belt of the surface of Mars, centered at 16 deg south latitude, show a very rugged terrain, with elevation differences greater than 13 kilometers from peak to valley. For nearby points, the relative altitude is measured to 40 meters at best; the precision is worse for points at different latitudes, or widely separated in longitude, because of orbital uncertainties. Some of the larger craters have been resolved, and their depth and, in some cases, the height of the raised rim have been measured. Where high resolution photographs are available, the correlation is excellent.

Downs, G. S.↗