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  • 1
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    Goldstone radar contributions to Mars Pathfinder landing safety (1994)
    In:  CASI
    Details
    Publication Date: 2013-08-31
    Description: Goldstar radar can provide topography 'profiles', statistical surface roughness, and radar images within a few degrees of the sub-Earth point. Goldstone/Very Large Array (VLA) bistatic radar observations can image the whole disk of Mars with integration times on the order of ten min before pixel smearing occurs. Data from all these radar techniques can be useful for observing the local surface conditions relating to landing safety issues for Mars Pathfinder.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst., Mars Pathfinder Landing Site Workshop; p 40
    Format: application/pdf
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  • 2
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    Mercury radar imaging - Evidence for polar ice (1992)
    In:  Other Sources
    Details
    Publication Date: 2019-08-28
    Description: The first unambiguous full-disk radar mapping of Mercury at 3.5-centimeter wavelength, with the Goldstone 70-meter antenna transmitting and 26 antennas of the Very Large Array receiving, has provided evidence for the presence of polar ice. The radar experiments, conducted on 8 and 23 August 1991, were designed to image the half of Mercury not photographed by Mariner 10. The orbital geometry allowed viewing beyond the north pole of Mercury; a highly reflective region was clearly visible on the north pole during both experiments. This polar region has areas in which the circular polarization ratio was 1.0 to 1.4; values less than about 0.1 are typical for terrestrial planets. Such high values of this ratio have hitherto been observed in radar observations only from icy regions of Mars and icy outer planet satellites.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Science (ISSN 0036-8075); 258; 5082; p. 635-640.
    Format: text
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  • 3
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    Radar images of Mars (1991)
    In:  Other Sources
    Details
    Publication Date: 2019-07-12
    Description: VLA radar-reflected flux-density mappings have yielded full disk images of Mars which reveal near-surface features, including a region in the Tharsis volcano area that displayed no echo to the very low level of the radar-system noise. This feature is interpreted as a deposit of dust or ash whose density is less than about 0.5 g/cu cm; it must be several meters thick, and may be much deeper. The most strongly reflecting geological feature was the south polar ice cap, which is interpretable as arising from nearly-pure CO2 or H2O ice, with less than 2 vol pct Martian dust. Only one anomalous reflecting feature was identified outside the Tharsis region.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Science (ISSN 0036-8075); 253; 1508-151
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  • 4
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    Radar reflectivity of Titan (1990)
    In:  Other Sources
    Details
    Publication Date: 2019-07-12
    Description: The low dielectric constant of the liquid hydrocarbon and ethane-methane surface mixture of Titan has as a direct consequence a set of unique microwave-reflection properties which were sought out at 3.5-cm wavelength, using a 70-m transmitting antenna in conjunction with the VLA as a receiving instrument. The statistically significant echoes obtained indicate that Titan is not covered with a deep global ocean of ethane. A global ocean as shallow as about 200 m would have exhibited reflectivities smaller by an order of magnitude, and below the experiment's detection limit.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Science (ISSN 0036-8075); 248; 975-980
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  • 5
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    Mercury - Full-disk radar images and the detection and stability of ice at the North Pole (1993)
    In:  Other Sources
    Details
    Publication Date: 2019-08-27
    Description: The first full-disk radar images of Mercury are discussed. About 77 percent of the surface was imaged at resolutions as good as 150 km. The North Pole was visible at the time of the observations, and the feature with the highest same sense (SS) circular reflectivity in the images is near the nominal polar position. The peak SS reflectivity of this feature is 7.9 percent and the circular polarization ratio through much of it is over one. The diameter of the feature is estimated to be less than about 350 km. The signal strength and polarization characteristics suggest the presence of very clean ices deposited in a relatively short period. The reflectivity of the north polar feature is slightly depressed compared to absolute reflectivities of other ice bodies and regions in the solar system. This may be due to a layer of dust or soil covering the ice. Other prominent features in the unphotographed hemisphere correpond to positions where atmospheric sodium enhancements have been measured from earth. These sites may be large basins similar to the Caloris basin.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Journal of Geophysical Research (ISSN 0148-0227); 98; E8; p. 15,003-15,023.
    Format: text
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