The attenuation of σ Arietis by the atmosphere of Jupiter during the occultation of November 20, 1952, was observed photoelectrically. Differential refraction in the upper stratospheric layers is shown to be the principal effect, and depends solely upon the geometry of the occultation and the scale height. The scale height in turn is a function of the ratio of the mean molecular weight of the atmosphere to its temperature. The best fit to the observations is obtained for a mean molecular weight barμ = 3.3, which is in substantial agreement with previous indirect estimates. The uncertainty, however, is such that it is not possible to distinguish between these estimates.
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Baum et al. (1953) studied this question.