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Volatile transport on Venus and implications for surface geochemistry and geologyThe high vapor pressure of volatile metal halides and chalcogenides (e.g., of Cu, Zn, Sn, Pb, As, Sb, Bi) at typical Venus surface temperatures, coupled with the altitude-dependent temperature gradient of approximately 8.5 K/km, is calculated to transport volatile metal vapors to the highlands of Venus, where condensation and accumulation will occur. The predicted geochemistry of volatile metals on Venus is supported by observations of CuCl in volcanic gases at Kilauea and Nyiragongo, and large enrichments of these and other volatile elements in terrestrial volcanic aerosols. A one-dimensional finite difference vapor transport model shows the diffusive migration of a thickness of 0.01 to greater than 10 microns/yr of moderately to highly volatile phases (e.g., metal halides and chalcogenides) from the hot lowlands (740 K) to the cold highlands (660 K) on Venus. The diffusive transport of volatile phases on Venus may explain the observed low emissivity of the Venusian highlands, hazes at 6-km altitude observed by two Pioneer Venus entry probes, and the Pioneer Venus entry probe anomalies at 12.5 km.
Document ID
19950050281
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Brackett, Robert A.
(Washington Univ. St. Luois, MS, United States)
Fegley, Bruce
(Washington Univ. St. Luois, MS, United States)
Arvidson, Raymond E.
(Washington Univ. St. Luois, MS, United States)
Date Acquired
August 16, 2013
Publication Date
January 25, 1995
Publication Information
Publication: Journal of Geophysical Research
Volume: 100
Issue: E1
ISSN: 0148-0227
Subject Category
Lunar And Planetary Exploration
Accession Number
95A81880
Funding Number(s)
CONTRACT_GRANT: NAGW-3446
CONTRACT_GRANT: NAGW-1358
CONTRACT_GRANT: NAGW-2867
Distribution Limits
Public
Copyright
Other

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