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Raman scattering in the atmospheres of the major planetsA technique is developed to calculate the detailed effects of Raman scattering in an inhomogeneous anisotropically scattering atmosphere. The technique is applied to evaluations of Raman scattering by H2 in the atmosphere of the major planets. It is noted that Raman scattering produces an insufficient decrease in the blue and ultraviolet regions to explain the albedos of all planets investigated. For all major planets, the filling-in of solar line cores and the generation of the Raman-shifted ghosts of the Fraunhofer spectrum are observed. With regard to Uranus and Neptune, Raman scattering is seen to exert a major influence on the formation and profile of strong red and near infrared CH4 bands, and Raman scattering by H2 explains the residual intensity in the cores of these bands. Raman scattering by H2 must also be taken into account in the scattering of photons into the cores of saturated absorption bands.
Document ID
19780038418
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Cochran, W. D.
(McDonald Observatory Austin, TX, United States)
Trafton, L. M.
(McDonald Observatory; Texas, University Austin, Tex., United States)
Date Acquired
August 9, 2013
Publication Date
January 15, 1978
Publication Information
Publication: Astrophysical Journal
Subject Category
Lunar And Planetary Exploration
Accession Number
78A22327
Funding Number(s)
CONTRACT_GRANT: NGR-44-012-152
Distribution Limits
Public
Copyright
Other

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