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The ionosphere of Venus - Observations and their interpretationThe implications of Soviet and U.S. observations of the Venus ionosphere's density, temperature, composition, motion, and magnetic structure are discussed, in view of the strong influence exerted on nearly all ionospheric parameters by the solar wind. The IMF conveys solar wind pressure to the ionosphere, compressing, accelerating, heating and removing plasma, forming the ionopause and inducing a nightward convection of plasma. Within the ionosphere, the main electron density peak is at an altitude of about 140 km on the day side, and is believed to be formed by local production and loss analogous to the earth's E region. Throughout most of the ionosphere, the nightward ion flow is primarily driven by the day-to-night pressure gradient, and electron precipitation also contributes to the nightside ionization. The lower atmosphere is dominated by O2(+), except at the lowest altitudes at night, where NO(+) and CO2(+) become significant ions.
Document ID
19830056206
Acquisition Source
Legacy CDMS
Document Type
Conference Proceedings
Authors
Brace, L. H.
(NASA Goddard Space Flight Center Greenbelt, MD, United States)
Taylor, H. A., Jr.
(NASA Goddard Space Flight Center Greenbelt, MD, United States)
Gombosi, T. I.
(Magyar Tudomanyos Akademia Kozponti Fizikai Kutato Intezet, Budapest, Hungary)
Kliore, A. J.
(California Institute of Technology, Jet Propulsion Laboratory, Pasadena CA, United States)
Knudsen, W. C.
(Lockheed Research Laboratories Palo Alto, CA, United States)
Nagy, A. F.
(Michigan, University Ann Arbor, MI, United States)
Date Acquired
August 11, 2013
Publication Date
January 1, 1983
Subject Category
Lunar And Planetary Exploration
Accession Number
83A37424
Distribution Limits
Public
Copyright
Other

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