Accurate and Consistent Microwave Observations of Venus and Their Implications

摘要: Abstract We present observations of Venus at six frequencies: 1.385, 1.465, 4.86, 8.44, 14.94, and 22.46 GHz. These were obtained with the Very Large Array calibrated in a consistent fashion. The brightness temperature frequencies is derived compared to model which includes emission from atmosphere, surface, subsurface Venus. A single set inputs can fit higher frequency data, where comes mostly atmosphere. At lower frequencies, surface subsurface, has difficulty reproducing measurements, lowest two are not reproduced well all. Improvements this over past models include new formalisms for microwave opacity SO 2 H 4 incorporation measured topography characteristics Magellan. best data relatively warm profile (more Mariner V occultation than that Pioneer–Venus sounders), disk-averaged abundance gaseous 1–2.5 ppm just below cloud layer, an average ⋦50 all altitudes layers. This values inferred Magellan occultations, taking into account differences between equatorial polar locations. atmosphere agreement earlier results P. G. Steffes, M. J. Klein, Jenkins (1990, Icarus 84, 83–92), but much 180 Pioneer sounder probe or 130 infrared observations. Models as measurements only if nearly completely devoid warmer by probes used.