The clouds are hazes of VenusPioneer Venus and Venera probe data for the clouds of Venus are considered. These clouds consist of a main cloud deck at 45-70 km altitude, with thinner hazes above and below, although the microphysical properties of the main cloud are further subdivided into upper, middle and lower cloud levels. Much of the cloud exhibits a multimodal particle size distribution, with the mode most visible from the earth being H2SO4 droplets having 2-3 micron diameters. Despite variations, the vertical structure of the clouds indicates persistent features at sites separated by years and by great distances. The clouds are more strongly affected by radiation than by latent heat release, and the small particle size and weak convective activity observed are incompatible with lightning of cloud origin.
Document ID
19830056199
Acquisition Source
Legacy CDMS
Document Type
Conference Proceedings
Authors
Esposito, L. W. (Colorado, University Boulder, CO, United States)
Knollenberg, R. G. (Particle Measuring Systems, Inc. Boulder, CO, United States)
Marov, M. IA. (Axademiia Nauk SSSR Moscow, Ussr)
Toon, O. B. (NASA Ames Research Center Moffett Field, CA, United States)
Turco, R. P. (R & D Associates Marina Del Rey, CA, United States)