Abstract
A model of the radiative portion of the equatorial atmosphere of Saturn, constrained by the infrared data various observers, has been constructed using a technique which includes the variation of thermal flux with depth. The model has a high-altitude temperature inversion due to the absorption of ultraviolet sunlight. The inversion causes the observed infrared emission peaks at 8 ωm (methane) and 12 ωm (ethane). Mixing ratios of these gases to hydrogen are computed from these emission features. The bottom of the modeled region occurs at the radiative-convective boundary. At this level, an opaque cloud consisting of solid ammonia condensation particles is postulated. Above the cloud is a thin haze, also composed of ammonia particles. The haze is required to match infrared observations near 9.5 ωm and hydrogen quadrupole equivalent widths near 0.64 ωm. Predictions of the model are given for further observational tests.
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