Interpretation of hydrogen quadrupole and methane observations of Jupiter and the radiative properties of the visible clouds.
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Hunt, G. E.↗
Engineering topics
Hunt, G. E.
Publications and source records attributed to Hunt, G. E..
Venus cloud cover.
It is shown that the presence of a cloud free region on Venus is not necessary for explaining the upward and downward atmospheric motions suggested by Goody and Robinson (1966) in the Venusian atmosphere. Considerations are given in support of the assumption that the cloud cover on Venus may be solid.
Bartlett, J. T.↗
Formation of spectral lines in planetary atmospheres. III - The use of analytic scattering diagrams in computations of synthetic spectra for cloudy atmospheres.
Results of some comparisons that have been made of line profiles and equivalent widths computed from atmospheric models where the scattering has been represented by the Mie theory and a simple analytic expression, the Heyney-Greenstein function. These results show that the spectroscopic features for these models are indistinguishable and demonstrate the value of using this simple analytic function in terms of the great saving in computer time when computing synthetic spectra for any cloudy planetary atmosphere.
Hunt, G. E.↗
Laboratory simulation of diffuse reflectivity from a cloudy planetary atmosphere.
For the first time measurements in the multiple scattering regime of the diffuse reflectivity as a function of single scattering albedo have been made in a geometry that may be simulated by a plane parallel atmosphere of large optical depth. A comparison between the measurements and a theoretical computation of the diffuse reflectivity is presented. The measurements are within 1% agreement with the theoretical calculations for two different sizes of scattering particles which are larger than and smaller than the wavelength of the incident light, corresponding to the Mie and Rayleigh regimes, respectively.
Margolis, J. S.↗
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.
Hunt, G. E.↗
Formation of spectral lines in a planetary atmosphere. II - Spectroscopic evidence for the structure of the visible Venus clouds.
We demonstrate in this article that there is spectroscopic evidence for the structure of the visible Venus cloud layers. From physically realistic models of the lower Venus atmosphere, we have shown that only observations of the phase variations of the CO2 bands in the Venus spectrum can provide the information for a unique identification of the structure of the cloud layers. It is proved that Venus cannot have a single dense cloud layer, but must have two scattering layers; a thin aerosol layer situated in the lower stratosphere, overlying a dense cloud deck. The aerosol plays an important role in the scattering of radiation, so that its identification provides an explanation of the reflecting layer-scattering model controversy for the interpretation of spectra formed in a cloudy planetary atmosphere.
Hunt, G. E.↗
Line formation in a Jovian atmosphere.
The nominal model of the Jovian atmosphere proposed by Divine (1970) is used as a basis for an interpretation of spectroscopic observations. The results discussed are concerned with those observations which may be quantitatively interpreted, i.e., the R-branch of the 3 nu sub 3 band of methane centered at 1.1 micron, and the hydrogen quadrupole spectrum. The results give a self-consistent model for the structure and composition of the atmosphere, and the radiative properties of the visible cloud layers.
Hunt, G. E.↗
The infrared spectrum of Jupiter - Structure and radiative properties of the clouds.
A model of the structure and radiative properties of the Jovian clouds is described that is inhomogeneous both laterally and vertically. Radiative transfer calculations are presented which include cloud effects and show that the model can account for available observations at all wavelengths.
Taylor, F. W.↗
Laboratory simulation of absorption spectra in cloudy atmospheres
Laboratory analog simulation of absorption line spectra in cloudy planetary atmospheres, comparing with computational model based on plane parallel atmosphere
Hunt, G. E.↗
Height variations of Venusian clouds
Height variations of Venusian cloud tops at planet equatorial and polar regions
Hunt, G. E.↗
A review of computational techniques for analysing the transfer of radiation through a model cloudy atmosphere
Model cloudy atmosphere construction, reviewing computational techniques for radiative transfer analysis
Hunt, G. E.↗