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Observational Constraints on Model Atmospheres for Uranus and Neptune

Published online by Cambridge University Press:  14 August 2015

Thérèse Encrenaz ,
Johannes Hardorp ,
Tobias Owen  and
Jerry H. Woodman
Thérèse Encrenaz
Affiliation:
Dept. of Earth and Space Sciences, State University of New York at Stony Brook, Stony Brook, N.Y., U.S.A.
Johannes Hardorp
Affiliation:
Dept. of Earth and Space Sciences, State University of New York at Stony Brook, Stony Brook, N.Y., U.S.A.
Tobias Owen
Affiliation:
Dept. of Earth and Space Sciences, State University of New York at Stony Brook, Stony Brook, N.Y., U.S.A.
Jerry H. Woodman
Affiliation:
McDonald Observatory, University of Texas, Fort Davis, Tex., U.S.A.

Abstract

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We have re-examined the visible and near-IR regions of the spectra of Uranus and Neptune to provide additional data for constructing atmospheric models. We find that a true continuum exists only at wavelengths below 4700 Å, that the 6420 Å absorption previously attributed to hydrogen is probably caused by methane, that there is no evidence for ammonia, ethylene or ethane absorptions in our spectra, and that the abundance of methane is probably much higher than previous estimates suggest. This last finding implies that the value of H/C in the atmospheres of both planets is much less than 1/10 the solar (or Jovian) value. Clear, Rayleigh-scattering model atmospheres are not compatible with the observations, but more work is needed to establish viable alternatives.

Type
Part III Outer Planets and Their Satellites
Information
Symposium - International Astronomical Union , Volume 65: Exploration of the Planetary System , 1974 , pp. 487 - 496
Copyright
Copyright © Reidel 1974 

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