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Venus cloud structure and water vapor abundance from Mariner 10 observationsObservations of the Venus atmosphere with the infrared radiometer on Mariner 10 have been analyzed by Taylor (1975) in terms of the vertical distribution of opacity at wavelengths near 11 microns and 45 microns in the thermal infrared. In this paper, we discuss models of the Venus atmosphere which are consistent with the inferred opacity structure. Either a two-layer cloud structure, or a single cloud deck overlaid by a layer containing approximately 40 precipitable microns of water vapor, would have the required limb-darkening characteristics at the wavelengths of observation.
Document ID
19770041241
Acquisition Source
Legacy CDMS
Document Type
Conference Proceedings
Authors
Taylor, F. W.
(California Institute of Technology, Jet Propulsion Laboratory, Planetary Atmospheres Section, Pasadena Calif., United States)
Date Acquired
August 8, 2013
Publication Date
January 1, 1976
Subject Category
Lunar And Planetary Exploration
Meeting Information
Meeting: Symposium and Workshop on Results from Coordinated Upper Atmosphere Measurement Programs
Start Date: May 29, 1975
End Date: May 31, 1975
Accession Number
77A24093
Funding Number(s)
CONTRACT_GRANT: NAS7-100
Distribution Limits
Public
Copyright
Other

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