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Formation of spectral lines in planetary atmospheres. I - Theory for cloudy atmospheres: Application to Venus.The theory of the formation of spectral lines in a cloudy planetary atmosphere is studied in detail. It is shown that models based upon homogeneous, isotropically scattering atmospheres cannot be used to reproduce observed spectroscopic features of phase effect and the shape of spectral lines for weak and strong bands. The theory must, therefore, be developed using an inhomogeneous (gravitational) model of a planetary atmosphere, accurately incorporating all the physical processes of radiative transfer. Such a model of the lower Venus atmosphere, consistent with our present knowledge, is constructed. The results discussed in this article demonstrate the effects of the parameters that describe the atmospheric model on the spectroscopic features of spectral line profile and phase effect, at visible and near infrared wavelengths. This information enables us to develop a comprehensive theory of line formation in a Venus atmosphere.
Document ID
19720039003
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
Authors
Hunt, G. E.
Date Acquired
August 6, 2013
Publication Date
March 1, 1972
Publication Information
Publication: Journal of Quantitative Spectroscopy and Radiative Transfer
Volume: 12
Subject Category
Space Sciences
Accession Number
72A22669
Distribution Limits
Public
Copyright
Other

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