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Distribution and source of the UV absorption in Venus' atmosphereThe model predictions were compared with the Pioneer Venus probes and orbiter to determine the composition of the UV absorbing materials. The simulations were carried out with radiative transfer codes which included spacecraft constraints on the aerosol and gas characteristics in the Venus atmosphere; gaseous SO2 (a source of opacity at the wavelengths below 0.32 microns), and a second absorber (which dominates above 0.32 microns) were required. The UV contrast variations are due to the optical depth changes in the upper haze layer producing brightness variations between equatorial and polar areas, and to differences in the depth over which the second UV absorber is depleted in the highest portion of the main clouds.
Document ID
19810042415
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
Authors
Pollack, J. B.
(NASA Ames Research Center Moffett Field, CA, United States)
Toon, O. B.
(NASA Ames Research Center Moffett Field, CA, United States)
Whitten, R. C.
(NASA Ames Research Center Moffett Field, CA, United States)
Boese, R.
(NASA Ames Research Center Moffett Field, CA, United States)
Ragent, B.
(NASA Ames Research Center Moffett Field, Calif., United States)
Tomasko, M.
(Arizona, University Tucson, Ariz., United States)
Esposito, L.
(Colorado, University Denver, Colo., United States)
Travis, L.
(NASA Goddard Institute for Space Studies New York, N.Y., United States)
Wiedman, D.
(Informatics, Inc. Palo Alto, Calif., United States)
Date Acquired
August 11, 2013
Publication Date
December 30, 1980
Publication Information
Publication: Journal of Geophysical Research
Volume: 85
Subject Category
Lunar And Planetary Exploration
Accession Number
81A26819
Distribution Limits
Public
Copyright
Other

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