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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...
The photometric detection of extrasolar planets by transits in eclipsing binary systems can be significantly improved by cross-correlating the observational light curves with synthetic models of possible planetary transit features, essentially a matched filter approach. We demonstrate the utility and application of this transit detection algorithm for ground-based detections of terrestrial-sized (Earth-to-Neptune...
Radio occultation experiments were conducted at Venus on three consecutive orbits of the Magellan spacecraft in October 1991. Each occultation occurred over the same topography (67 o N, 127 o E) and at the same local time (22 h 5 m ), but the data are sensitive to zonal variations because the atmosphere rotates significantly during one orbit. Through comparisons between...
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