Computer Science
Scientific paper
May 1991
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991spfl...33..156m&link_type=abstract
Spaceflight (ISSN 0038-6340), vol. 33, May 1991, p. 156-160.
Computer Science
Planetary Crusts, Planetary Geology, Planetary Mapping, Topography, Venus (Planet), Geochronology, Magellan Project (Nasa), Radar Maps, Synthetic Aperture Radar, Tectonics, Venus, Geology, Surface, Features, Spacecraft Observations, Ejecta, Magellan Mission, Radar Methods, Sar Instrument, Mapping, Meteoroids, Mission Description, Technical Aspects, Topography, Crust, Hypotheses, Thickness, Tectonism, Deformation, Rift Zones, Comparisons, Mountains, Ridges, Tesserae, Volcanism, Eruptions, Impacts, Craters, D
Scientific paper
The Magellan mission to Venus is reviewed. The scientific investigations conducted by 243-day cycles encompass mapping with a constant incidence angle for the radar, observing surface changes from one cycle to the next, and targeting young-looking volcanos. The topography of Venus is defined by the upper boundary of the crust and upwelling from lower domains. Tectonic features such as rift zones, linear mountain belts, ridge belts, and tesserae are described. The zones of tesserae are unique to the planet. Volcanism accounts for about 80 percent of the observed surface, the remainder being volcanic deposits which have been reworked by tectonism or impacts. Magellan data reveal about 900 impact craters with flow-like ejecta resulting from the fall of meteoroids. It is concluded that the age of the Venusian surface varies between 0 and 800 million years. Tectonic and volcanic activities dominate the formation of the Venus topography; such processes as weathering and erosion are relatively unimportant on Venus.
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