Radar Mapping of Venus With Interf Erometric Resolution of the Range‐Doppler Ambiguity

Rogers, A. E. E.; Ingalls, R. P.

doi:10.1029/rs005i002p00425

Cited by 25 publications

(7 citation statements)

References 4 publications

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“…Feature a is in the southeast, and j3 and 7 are composed of three separate rounded features, each about 150 miles across [Goldstein, 1970]. There is a small dark area below the center of the disk and a dark area with a central peak near feature a Rogers and Ingalls, 1970]. The bulk of the surface of Venus is significantly smoother than the surface of the moon [Jurgens, 1970].…”

Section: Surface Of Venusmentioning

confidence: 99%

The surfaces of solar‐system bodies

Huguenin

McCord

1971

EoS Transactions

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Extensive study of the lunar surface using spacecraft (Ranger, Surveyor, Orbitor, and Apollo projects) and a surge of activity at visible, IR, and radio wavelengths using ground‐based telescopes during the past 5 years has resulted in a staggering increase in knowledge of the moon. It is impossible to cover properly even the major results in this limited format. We give here a very abbreviated discussion and refer the interested reader to the project reports and review articles listed in the first section of the bibliography. Individual references in the text are not given when the topic is covered in the appropriate mission report, usually by several authors. Articles that appeared separately in the literature are referenced in the text. The bibliography contains only articles that appear in major scientific journals. Again the extent of the literature has required extensive, and perhaps some improper, deletions.

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Section: Surface Of Venusmentioning

confidence: 99%

The surfaces of solar‐system bodies

Huguenin

McCord

1971

EoS Transactions

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“…For more distant celestial objects, the antenna beam may not resolve the two hemispheres, and another solution to the ambiguity problem must be found. For instance, Roger and Ingalls [19] used a radar interferometer in order to obtain unambiguous images of Venus. By analyzing the signals at both receive antennas, they were able to separate contributions from points on both hemispheres.…”

Section: A Delay-doppler Mappingmentioning

confidence: 99%

“…The 85-km diameter crater Tycho (43 S, 349 E), the youngest large crater on the Moon, was imaged on October 19,1997. A 200 200-km delay-Doppler image of the Tycho region is shown in Fig.…”

Section: A Tycho Cratermentioning

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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“…To accomplish this, the two ambiguous cells are assumed to lie on the mean spherical surface, and their associated phase angles are then equal but opposite in sign. Rogers and Ingalls [1970] demonstrated that power from the northern and southern hemispheres could be separated easily except for regions where the fringe phase angle is multiples of ,r rad. Campbell et al [1970] used the same procedure to construct maps of Venus with the Arecibo radar telescope at 70-cm wavelength.…”

Section: Introduction and Historymentioning

confidence: 99%

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

Jurgens¹,

Goldstein²,

Rumsey³

et al. 1980

J. Geophys. Res.

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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.

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Radar Mapping of Venus With Interf Erometric Resolution of the Range‐Doppler Ambiguity

Cited by 25 publications

References 4 publications

The surfaces of solar‐system bodies

The surfaces of solar‐system bodies

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

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

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