Images of Venus by three‐station radar interferometry—1977 results

Jurgens, R. F.; Goldstein, Robert S.; Rumsey, Howard; Green, R. R.

doi:10.1029/ja085ia13p08282

Cited by 19 publications

(6 citation statements)

References 14 publications

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“…What are the surface characteristics that produce such variable signatures in this volcanic terrain? Goldstone incidence angles for most of these features are in the 5°-70 range, for which differences in rms slopes are expected to have minimal effects on backsca[[er strength (the Hagfors "crossover" region [Jurgens et al, 1980]). In the absence of large topographic gradients, backscatter variations in this Goldstone image are most likely due to differences in dielectric Conslant.…”

Section: Volcanic Terrain In Navka Planitiamentioning

confidence: 99%

Comparison of Goldstone and Magellan radar data in the equatorial plains of Venus

Plaut¹,

Arvidson²

1992

J. Geophys. Res.

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Goldstone radar observations of the equatorial plains of Venus provide complementary information to that obtained by Magellan. Different radar scattering mechanisms dominate each system, leading to a sampling of different surface properties. Comparison of image data and derived parameters indicate that (1) relatively high dielectric constants on impact‐related parabolic features are detected in Goldstone backscatter, Magellan reflectivity, and Magellan emissivity data; the dielectric effects are overwhelmed by roughness‐related signatures in Magellan synthetic aperature radar (SAR) data, (2) lava flows in Navka Planitia show dielectric variations both among and within flows; higher dielectric constants on the perimeter of some flows may be due to a decrease in vesicularity, (3) some volcanic domes are relatively smooth at the wavelength scale and probably consist of low‐density deposits, (4) comparisons of Magellan SAR data with rough surface scattering models and SAR data of terrestrial surfaces indicate that the roughness characteristics of the equatorial plains surfaces are comparable to modified terrestrial lava flows, and (5) scattering properties of an equatorial “ridge belt” structure suggest highly weathered or soil‐dominated surfaces.

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Section: Volcanic Terrain In Navka Planitiamentioning

confidence: 99%

Comparison of Goldstone and Magellan radar data in the equatorial plains of Venus

Plaut¹,

Arvidson²

1992

J. Geophys. Res.

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“…4.1). The theory and data processing operations of three station interferometry for obtaining the topography is described in Jurgens et al (1980). The standard error of their altimetry is about 35 m near the sub-radar point increasing to about one kilometer at 6°.…”

Section: Earth-based Radar Observations Of the Surfacementioning

confidence: 99%

The geology of the terrestrial planets

Carr¹

1983

Reviews of Geophysics

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During the last four years our knowledge of the geology of the terrestrial planets has advanced rapidly. The advances are particularly noticeable for Venus and Mars. Improved understanding of Venus has come largely from the Pioneer Venus mission (Colin, 1980), which has given us our first global view of the planet, albeit at fairly low resolution. The period was also one of almost continuous data gathering for Mars as the Viking orbiters and landers, emplaced at the planet in 1976, continued to function.

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“…By analyzing the signals at both receive antennas, they were able to separate contributions from points on both hemispheres. Their use of an interferometer was not related to the measurement of elevations, but later extensions of the technique [20], [21] did provide altitude contours.…”

Section: A Delay-doppler Mappingmentioning

confidence: 99%

Digital elevation models of the Moon from Earth-based radar interferometry

Margot

Campbell

Jurgens

et al. 2000

IEEE Trans. Geosci. Remote Sensing

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Three-dimensional (3-D) maps of the nearside and polar regions of the Moon can be obtained with an Earth-based radar interferometer. This paper describes the theoretical background, experimental setup, and processing techniques for a sequence of observations performed with the Goldstone Solar System Radar in 1997. These data provide radar imagery and digital elevation models of the polar areas and other small regions at 100 m spatial and 50 m height resolutions. A geocoding procedure relying on the elevation measurements yields cartographically accurate products that are free of geometric distortions such as foreshortening. He is currently a Research Associate at the Arecibo Observatory, Arecibo, PR, where he is involved in planetary studies and remote sensing. He has previously worked on the measurement of atmospheric water content from microwave observations and on characterizing the lunar regolith via multiwavelength polarimetric radar and radio observations. His current research interests include the study of scattering from planetary surfaces, the use of radar interferometry for topographic mapping and surface change detection, and the inversion of delay-Doppler data for shape reconstruction. He is also pursuing the implementation of two-element radar interferometry techniques for the unambiguous imaging and the three-dimensional characterization of small bodies.

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Images of Venus by three‐station radar interferometry—1977 results

Cited by 19 publications

References 14 publications

Comparison of Goldstone and Magellan radar data in the equatorial plains of Venus

Comparison of Goldstone and Magellan radar data in the equatorial plains of Venus

The geology of the terrestrial planets

Digital elevation models of the Moon from Earth-based radar interferometry

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