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Science 12 April 1991:
Vol. 252. no. 5003, pp. 276 - 288
DOI: 10.1126/science.252.5003.276
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Articles
Venus Volcanism: Initial Analysis from Magellan Data
JAMES W. HEAD 1,
DONALD B. CAMPBELL 2,
CHARLES ELACHI 3,
JOHN E. GUEST 4,
DAN P. MCKENZIE 5,
R. STEPHEN SAUNDERS 3,
GERALD G. SCHABER 6, and
GERALD SCHUBERT 7
1 Department of Geological Sciences, Brown University, Providence, Rhode Island 02912
2 Department of Astronomy, Cornell University, Ithaca, NY 14853
3 Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, CA 91109
4 University of London Observatory, University College London, Mill Hill Park, London, England NW72QS
5 Bullard Laboratories, Department of Earth Sciences, Cambridge University, Cambridge, England CB3OEZ
6 U.S. Geological Survey, 2255 North Gemini Drive, Flagstaff, AZ 86001
7 Department of Earth and Space Sciences, Institute of Geophysics and Planetary Physics, University of California at Los Angeles, Los Angeles, CA 90024
Magellan images confirm that volcanism is widespread and has been fimdamentally important in the formation and evolution of the crust of Venus. High-resolution imaging data reveal evidence for intrusion (dike formation and cryptodomes) and extrusion (a wide range of lava flows). Also observed are thousands of small shield volcanoes, larger edifices up to several hundred kilometers in diameter, massive outpourings of lavas, and local pyroclastic deposits. Although most features are consistent with basaltic compositions, a number of large pancake-like domes are morphologically similar to rhyolite-dacite domes on Earth. Flows and sinuous channels with lengths of many hundreds of kilometers suggest that extremely high effusion rates or very fluid magmas (perhaps komatiites) may be present. Volcanism is evident in various tectonic settings (coronae, linear extensional and compressional zones, mountain belts, upland rises, highland plateaus, and tesserae). Volcanic resurfacing rates appear to be low (less than 2 Km3/yr) but the significance of dike formation and intrusions, and the mode of crustal formation and loss remain to be established.
Submitted on January 22, 1991
Accepted on March 20, 1991
THIS ARTICLE HAS BEEN CITED BY OTHER ARTICLES:
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