Engineering topics

Campbell, D. B.

Publications and source records attributed to Campbell, D. B..

At least 73 records · Page 4

NASA NTRS1983

Radar observations of asteroid 1685 Toro

The present results of 13 cm wavelength radar observations of the asteroid 1685 Toro, conducted at the Arecibo Observatory in July 1980, yield radar spectra which reveal correlated and approximately twofold variations in radar cross section and spectral bandwidth as functions of rotational phase, with two maxima and two minima per rotation cycle. In combination with the photopolarimetric results of Dunlap et al. (1973), the observations presently reported offer constraints on Toro's size, shape, and surface properties. Modeling Toro as a homogeneously scattering ellipsoid yields weighed least squares estimates for the lengths of the equatorial semiaxes and a nearly Lambertian scattering law.

Ostro, S. J.↗

NASA NTRS1982

Comet Encke - Radar detection of nucleus

The nucleus of the periodic comet Encke was detected in November 1980 with the Arecibo Observatory's radar system (wavelength, 12.6 cm). The echoes in the one sense of circular polarization received imply a radar cross section of 1.1 + or - 0.7 sq km. The estimated bandwidth of these echoes combined with an estimate of the rotation vector of Encke yields a radius for the nucleus of 1.5 +2.3 or -1.0. The uncertainties given are dependent primarily on the range of models considered for the comet and for the manner in which its nucleus backscatters radio waves. Should this range prove inadequate, the true value of the radius of the nucleus might lie outside the limits given.

Kamoun, P. G.↗

NASA NTRS1982

Delay-Doppler radar observations of Saturn's rings

Delay-Doppler observations at 12.6 cm which have been used to estimate the relative radar reflectivities of Saturn's classical ring sections show that the A and B rings are responsible for most of the radar echo, and that the average radar reflectivity per unit of projected area of the A ring is 90% as large as the B ring. No firm evidence is found for radar backscattering from particles interior to the B ring, exterior to the A ring, of from the planet itself. Unexpectedly large amounts of power at Doppler shifts near the center of the echo spectrum, which had been reported at 3.5 and 12.6 cm for ring plane tilt angles greater than 24.4 deg are not apparent in spectra for those wavelengths obtained at ring plane tilt angles smaller than 21.4 deg.

Ostro, S. J.↗

NASA NTRS1980

Radar observations of the icy Galilean satellites

It is shown that when combined with previous observations, 12.6 cm radar observations of Europa, Ganymede and Callisto made at the Arecibo Observatory in November 1977 and February 1979 firmly establish the distinguishing radar properties of the satellites: (1) high geometric albedos, (2) circular polarization ratios which anomalously exceed unity, (3) linear polarization ratios of approximately 0.5, and (4) diffuse scattering, which varies with the cosine of the angle of incidence. The weighted-mean values of these properties are tabulated, and it is found that although significant albedo and/or polarization features are common in the radar spectra, the fractional root mean square fluctuations in disk-integrated properties is only about 10%.

Ostro, S. J.↗

NASA NTRS1980

Radar detection of Vesta

Asteroid 4 Vesta was detected on November 6, 1979 with the Arecibo Observatory's S-band (12.6-cm-wavelength) radar. The echo power spectrum, received in the circular polarization opposite to that transmitted, yields a radar cross section of (0.2 + or - 0.1)pi a-squared, for a = 272 km. The data are too noisy to permit derivation of Vesta's rotation period.

Ostro, S. J.↗

NASA NTRS1980

Radar observations of Saturn's rings at intermediate tilt angles

The 12.6-cm-wavelength radar observations of Saturn's rings, corresponding to ring-plane tilt angles of 18.2, 11.7, and 5.6 degrees, respectively, are reported. Measurements of geometric albedo and circular polarization ratio are used to investigate acceptable ring models and radar scattering properties of individual particles. Attention is given to the dependence of the rings' polarization properties on wavelength or tilt angle, or both. All large-particle monolayer models of Saturn's rings are ruled out; however, extended-layer models postulating ice or metal particles are compatible with the radar albedo measurements and are less severely restricted by the polarization data.

Ostro, S. J.↗

NASA NTRS1979

Radar observations of asteroid 1580 Betulia

Radar observations of the asteroid 1580 Betulia, made at a wavelength of 12.6 cm, show a mean radar cross section of 2.2 + or- 0.8 sq km and a total spectral bandwidth of 26.5 + or- 1.5 Hz. Combining bandwidth measurements with the optically determined rotation period sets a lower limit to the asteroid's radius of 2.9 + or- 0.2 km.

Pettengill, G. H.↗

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 NTRS1979

Nonresonance rotation of Venus

Radar observations accumulated over the past 14 yr are used to make a precise estimate of the spin vector of Venus. The results obtained show that the spin vector of Venus may be adequately described in the standard 1950.0 coordinate system by a period of 243.01 + or - 0.03 days (retrograde) and a north pole direction corresponding to alpha = 272.8 + or - 0.5 deg and delta = 67.2 + or - 0.3 deg; the quoted errors represent estimates of 70% confidence intervals. The angular separations between the spin vector and those vectors representing the unit normals to the invariable plane of the solar system and the orbital plane of Venus are found to be 0.5 deg and 2.6 deg, respectively. It is concluded that Venus is not rotating with a resonance spin period relative to the orbit of earth and that the spin of Venus may be in a generalized Cassini state.

Shapiro, I. I.↗

NASA NTRS1978

Arecibo radar observations of Mars surface characteristics in the Northern Hemisphere

Mars surface characteristics at and near the Viking Chryse and Tritonis Lacus landing areas were determined by radio scatter using the 12.6-cm radar at the Arecibo Observatory during 1975-76. Interpretation of each power spectrum suggests rms surface tilts of 4 deg at the final A1WNW (47.9 deg W, 22.5 deg N) site, 5 deg near the original A1 site, and 6 deg between the two. At the back-up site (A2) surface-roughness estimates were about 4 deg. Striking changes in surface texture have been found near the eastern bases of Tharsis Montes and Albor Tholus, each volcanic feature marking the western boundary of very smooth surface units. The roughness sensed at 1- to 100-m scales by radar appears to be relatively independent of the surface units defined at large scale lengths by photogeologists. Radar properties thus provide an additional means by which planetary surfaces may be characterized.

Simpson, R. A.↗

NASA NTRS1978

Galilean satellites - 1976 radar results

In addition to a report of radar observations concerning the Galilean satellites made in the fall of 1976, Doppler results are presented from 1975 and January 1976. The primary objectives of the investigation conducted in 1976 are related to a study of each satellite at widely separated orbital phases and a close examination of the polarization of its scattered energy. The investigation included an observation of Io, Europa, Ganymede, and Callisto with the upgraded Arecibo S-band radar system on 11 nights irregularly distributed from 26 October 1976 to 7 December 1976. Several peculiarities revealed by the radar observations of the three outer Galilean satellites are related to large and possibly time-varying albedos, and the unexpected result that the circular polarization transmitted exceeds unity by a substantial amount.

Campbell, D. B.↗

NASA NTRS1978

Arecibo radar observations of Martian surface characteristics near the equator

Mars radar observations at 12.6-cm wavelength indicate that many of what were potential Viking landing sites along the planet's equator are rougher than interpretations of Mariner 9 images suggested. Root mean square surface slopes are typically 5 degrees in the region bounded by 160 and 200 degrees W, 0 and 12 degrees S. From Tharsis Montes west to 160 degrees W, radar-scattering characteristics suggest extreme roughness on small scales, perhaps exceeding 10 degrees in rms magnitude. East of Tharsis and north of Valles Marineris the surface is smooth, with values of rms slope as low as 1 degree; the elevation of this plateau was too high for a Viking landing. Study of spectral shapes indicates the Hagfors scattering law remains the best descriptor of quasi-specular surface scattering properties in an average sense; widespread variations in the surface argue against its indiscriminate use, however. Backscattering at moderate (25-40 degrees) incidence angles was studied qualitatively and was found to be significantly above the level predicted by a strictly quasi-specular (e.g., Hagfors) process; it also is variable over the surface.

Simpson, R. A.↗

NASA NTRS1977

Galilean satellites of Jupiter - 12.6-centimeter radar observations

The newly improved 12.6-cm Arecibo radar system on Puerto Rico was employed in a study of the Galilean satellites, conducted during the time between September 28 and November 1, 1975. An additional night was assigned for observing Io on January 16, 1976. The radar cross sections obtained for Europa, Ganymede, and Callisto show nearly the same relative values as do the optical cross sections. Radar scattering spectra are presented in graphs. A table with the results of the radar investigations is also provided.

Campbell, D. B.↗

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

New radar image of Venus

The paper discusses a new radar image of the visible face of Venus, with particular reference to the relative backscattered power between latitudes 46 and 75 deg and covering the approximate longitude range from 290 to 10 deg, with an approximate resolution of 20 km. Two features seem to dominate this region: one is a large low-contrast area with a well-defined rim on its southern side and with two high-contrast features forming its northern and northwestern edges, and the other consists of the same two small high-contrast features on the northern edge of the basin and a large very high contrast feature straddling the zero-deg meridian and extending from 60 to 70 latitude, the last feature being previously named Maxwell. It is shown that Maxwell and the two high-contrast features are likely to indicate tectonic activity. Their probable high degree of surface roughness, well-defined boundaries, and irregular shapes make an origin based on the impact history of the planet hard to conceive.

Campbell, D. B.↗

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 NTRS1976

70-cm radar observations of 433 Eros

Radar observations of 433 Eros were made at the Arecibo Observatory using a wavelength of 70 cm during the close approach of Eros to earth in mid-January, 1975. A peak radar cross section of plus or minus 15 sq km was observed. The spectral broadening obtained was approximately 30 Hz, which is consistent with a value of 16 km for the maximum radius of the asteroid. The surface of Eros appears to be relatively rough at the scale of a wavelength as compared to the surfaces of the terrestrial planets and the moon. The composition of the surface is not well determined, except that it cannot be a highly conducting metal. A single measurement each of round-trip echo times delay and Doppler shift was made.

Campbell, D. B.↗

NASA NTRS1975

Pulsar fluctuation spectra and the generalized drifting-subpulse phenomenon. II

Pulsar observations at meter wavelengths have been analyzed to investigate pulse-to-pulse variations and to identify regions of the pulse profile which display distinct statistical properties. Fluctuation spectra of eight recently discovered pulsars are presented along with a description of the drifting-subpulse phenomenon in several objects with quasiperiodic responses in their fluctuation spectra. A quantitative analysis of the drifting-subpulse phenomenon in PSR 0031-07 and PSR 0809+74 is given which emphasizes the broad-band nature of the phenomenon. A summary of the memory exhibited by pulsars with time scales of about 50 periods is given.

Backer, D. C.↗