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Radiative equilibrium models of the Jovian atmosphere calculated by Hogan, Rasool, and Encrenaz (1969) and by Cess and Khetan (1973) are shown to be in conflict. A new calculation is presented which agrees closely with that of Cess and Khetan. This model, however, fails to predict the observed intensity in the 7.8-micron methane band by about a factor of 8. It is shown that the observed emission intensity in the 7.8-micron band is a critical test of these models. The Pioneer 10 occultation profile is at variance with the models. The emission intensity at 7.8 microns implied by the Pioneer 10 result is shown to be 100 times greater than observed. It is concluded that the Pioneer 10 temperature profile is not representative of the global average.-

The equation of radiative transfer for a Rayleigh scattering atmosphere including polarization is reduced to an azimuth-independent form. The integro-differential equations are then solved by approximating the integrals as sums and the differentials as finite differences. The resultant set of equations is then solved by the Feautrier technique. This method can solve inhomogeneous atmospheres by allowing for arbitrary variations with depth of the single scattering albedo and the source term. As an example, zero-phase geometric albedos and center-to-limb intensities are calculated for a planetary disk with a semi-infinite pressure-induced absorbing atmosphere.