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A multi-wavelength radio frequency observation of Venus was performed on April 5, 1996, with the Very Large Array to investigate potential variations in the vertical and horizontal distribution of temperature and the sulfur compounds sulfur dioxide (SO 2 ) and sulfuric acid vapor (H 2 SO 4 (g)) in the atmosphere of the planet. Brightness temperature maps were produced which...
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 and calibrated in a consistent fashion. The brightness temperature of Venus at the six frequencies is derived and compared to a model which includes the emission from the atmosphere, surface, and subsurface of Venus. A single set of model inputs can fit...
New abundance profiles of gaseous sulfuric acid (H 2 SO 4 ) have been computed based on the measured absorptivity profiles of the Venus atmosphere obtained during the 1991–1992 Magellan radio occultation experiments (975887;975887) and the 1974 Mariner 10 radio occultation experiment (975887). The Magellan abundance profiles are different than those previously reported by Jenkinset...