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Light scattering by an optically thin inhomogeneous, spherically-symmetric planetary atmosphere: Brightness at the zenith near the terminator

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Abstract

The approximate method of representing the intensity by a three-stream angular division is used to compute the brightness at the zenith near the terminator of an optically thin, spherically-symmetric planetary atmosphere illuminated by parallel solar radiation. The results are compared with those of Sobolev obtained under classical Eddington approximation.

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References

  • Sobolev V. V.: 1975,Light Scattering in Planetary Atmospheres, Pergamon Press, Oxford.

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  • Unno W. and Kondo M.: 1976,Publ. Astron. Soc. Japan 28, 347.

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  • Wilson, S. J. and Sen K. K.: 1980,Astrophys. Space Sci. 69, 107.

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Authors and Affiliations

  1. Department of Mathematics, University of Singapore, Republic of Singapore

    S. J. Wilson & K. K. Sen

Authors
  1. S. J. Wilson
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  2. K. K. Sen
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Additional information

Part of this work was done when the author was on sabbatical leave at Kanazawa Institute of Technology (Japan).

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Wilson, S.J., Sen, K.K. Light scattering by an optically thin inhomogeneous, spherically-symmetric planetary atmosphere: Brightness at the zenith near the terminator. Astrophys Space Sci 71, 405–410 (1980). https://doi.org/10.1007/BF00639400

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  • DOI: https://doi.org/10.1007/BF00639400

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