Abstract
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.
Guest investigator, Hale Observatories, 1972.
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Encrenaz, T., Hardorp, J., Owen, T., Woodman, J.H. (1974). Observational Constraints on Model Atmospheres for Uranus and Neptune. In: Woszczyk, A., Iwaniszewska, C. (eds) Exploration of the Planetary System. International Astronomical Union/Union Astronomique Internationale, vol 65. Springer, Dordrecht. https://doi.org/10.1007/978-94-010-2206-4_44
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DOI: https://doi.org/10.1007/978-94-010-2206-4_44
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