Physics
Scientific paper
Jan 1980
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980sci...207..289k&link_type=abstract
Science, vol. 207, Jan. 18, 1980, p. 289-293.
Physics
Pioneer Venus Spacecraft, Venus Atmosphere, Venus Surface, Abundance, Argon, Satellite Observation, Spectrum Analysis, Venus, Pioneer Venus, Comparisons, Earth, Physical Properties, Geology, Chemical Properties, Volatile Elements, Rare Gases, Argon, Evolution, Temperatures, Cosmic Dust, Scattering, Models, Surface Features, Radar Mapping, Craters, Terrain, Volcanic Features, Tectonic Activity, Atmosphere, Winds, Clouds, Sulfur Cycle, Thermodynamics, Water Vapor, Greenhouse Effect, Heat, Circulation
Scientific paper
Some of the data obtained as a result of the Pioneer Venus mission, a combination of an orbiter and five atmospheric probes, are detailed and their possible interpretations are discussed. The discovery of large amounts of argon-36 in the Venusian atmosphere disproved the hypothesis that amounts of inert gases could be used to estimate the amounts of volatile reactive elements, which could be chemically tied up within the planet. It now seems that the amounts of carbon, hydrogen and nitrogen are not linked to the amounts of inert gases. The mapping of the surface of Venus by the Pioneer orbiter's radar confirmed the variety of surface features deduced from the ground-based data. Although some surface features of Venus can be compared with some on Earth or Mars (hills, ridges, plateaus, volcanoes, and mountains up to 12 km high), the scarcity of basins (15 to 20 percent compared to 70 percent on Earth) suggests a special kind of tectonic activity on Venus. Still many questions about Venus remain unanswered, in particular, questions related to its atmosphere: e.g. the 360 kmph winds that carry the cloud tops around the entire planet in 4 days, the cycling of sulfur through the clouds and atmosphere, or the 460 C temperature at the bottom of the atmosphere.
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