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Observations of jupiter'S cloud structure near 8.5 μ

Published online by Cambridge University Press:  14 August 2015

J. A. Westphal
J. A. Westphal*
Affiliation:
Mt. Wilson and Palomar Observatories, Carnegie Institution of Washington, California Institute of Technology and Division of Geological Sciences, California Institute of Technology, Pasadena, Calif., U.S.A.

Abstract

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Measurements of the distribution of thermal flux along polar and equatorial scans across Jupiter suggest that the increase in brightness temperature near 8.5 μ observed by Gillett et al. may be caused by flux coming from near the cloud tops. Other possible sources are discussed and observational tests suggested which should clarify the thermal structure of the upper atmosphere.

Type
Part III: Outer Planets
Information
Symposium - International Astronomical Union , Volume 40: Planetary Atmospheres , 1971 , pp. 359 - 362
Copyright
Copyright © Reidel 1971 

References

Gillett, F. C., Low, F. J., and Stein, W. A.: 1969, Astrophys. J. 157, 925.Google Scholar
Ingersoll, A. P. and Cuzzi, J. N.: 1969, J. Atmospheric Sci. Google Scholar
Trafton, L. M.: 1967, Astrophys. J. 147, 765.Google Scholar
Westphal, J. A.: 1969, Astrophys. J. 157, L63.Google Scholar