The composition of the atmosphere of Venus below 100 km altitude: An overview |
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| Institution: | 1. Lunar and Planetary Institute, 3600 Bay Area Boulevard, Houston, TX 77586, USA\n;2. Department of Earth Sciences, Simon Fraser University, 8888 University Drive, Burnaby, British Columbia V5A 1S6, Canada\n;1. Department of Physics, Catholic University of America, Washington, DC 20064, USA;2. Moscow Institute of Physics and Technology (PhysTech), Dolgoprudnyy 141700, Russia;1. Department of Physics, South Dakota State University, Brookings, SD 57007, United States of America |
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| Abstract: | We review the progress in our understanding of the composition of the Venus atmosphere since the publication of the COSPAR Venus International Reference Atmosphere volume in 1985. Results presented there were derived from data compiled in 1982–1983. More recent progress has resulted in large part from Earth-based studies of the near-infrared radiation from the nightside of the planet. These observations allow us to probe the atmosphere between the cloud tops and the surface. Additional insight has been gained through: (i) the analysis of ultraviolet radiation by satellites and rockets; (ii) data collected by the Vega 1 and 2 landers; (iii) complementary analyses of Venera 15 and 16 data; (iv) ground-based and Magellan radio occultation measurements, and (v) re-analyses of some spacecraft measurements made before 1983, in particular the Pioneer Venus and Venera 11, 13 and 14 data. These new data, and re-interpretations of older data, provide a much better knowledge of the vertical profile of water vapor, and more information on sulfur species above and below the clouds, including firm detections of OCS and SO. In addition, some spatial and/or temporal variations have been observed for CO, H2O, H2SO4, SO2, and OCS. New values of the D/H ratio have also been obtained. |
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