Magellan: Electrical and Physical Properties of Venus' Surface

Magellan probes Venus' surface by 12.6-cm-wavelength vertical and oblique radar scattering and measures microwave thermal emission. Emissivity and root-mean-square slope maps between 330° and 30°E and 90°N and 80°S are dissimilar, although some local features are exceptions. Inferred surface em...

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Bibliographic Details
Published in:Science (American Association for the Advancement of Science) 1991-04, Vol.252 (5003), p.265-270
Main Authors: Tyler, G. Leonard, Ford, Peter G., Campbell, Donald B., Elachi, Charles, Pettengill, Gordon H., Simpson, Richard A.
Format: Article
Language:English
Subjects:
Altimeters
Altitude
Angle of incidence
Antennas
Earth sciences
Electricity
Emissivity
Geology
Lunar And Planetary Exploration
Radar
Radar echoes
Radar in earth sciences
Radar systems
Reflectance
Space exploration
Spacecraft
Surface (Geology)
Venus
Venus (Planet)
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Summary:Magellan probes Venus' surface by 12.6-cm-wavelength vertical and oblique radar scattering and measures microwave thermal emission. Emissivity and root-mean-square slope maps between 330° and 30°E and 90°N and 80°S are dissimilar, although some local features are exceptions. Inferred surface emissivities typically are ∼0.85, but vary from ∼0.35 at Maxwell to ∼0.95 northeast of Gula Mons and other locations. Lowest emissivities appear in topographically high areas; this relation suggests that a phase change or differences in chemical weathering occur at about 6055-kilometer radius. Initial results indicate that there are significant variations in the surface scattering function.
ISSN:0036-8075
1095-9203
DOI:10.1126/science.252.5003.265