Structure of the atmospheres of Mars and Venus below 100 kilometers |
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| Institution: | 1. NASA Langley Research Center, Hampton, VA 23665-5225, U.S.A.;2. University of Utah, Department of Mechanical Engineering, Salt Lake City, UT 84112, U.S.A.;3. United States Geological Survey, Flagstaff, AZ 86001, U.S.A.;4. Jet Propulsion Laboratory, Pasadena, CA 91109, U.S.A.;1. Max-Planck-Institut für Sonnensystemforschung, Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany;2. Physical Faculty, Moscow State University, 119992 GSP-2 Lengory, Moscow, Russia;3. Institute of Radio-engineering and Electronics, ulitza Mokhovaya, 11/7, 125009 Moscow, Russia;4. The All-Russian Research Institute for Optical and Physical Measurements (VNIIOFI), 119361 Moscow, Ozernaya, Russia;1. UNESP-Grupo de Dinâmica Orbital e Planetologia, Guaratinguetá, SP 12516-410, Brazil;2. Instituto Nacional de Pesquisas Espaciais, Av. dos Astronautas 1758, São José dos Campos, SP 12227-010, Brazil;3. Departament de Matemàtica Aplicada I, ETSEIB-UPC, Avda. Diagonal 647, 08028 Barcelona, Spain;4. Departament de Matemàtica Aplicada i Anàlisi, UB, Gran Vía 585, 08007 Barcelona, Spain;1. Institute of Space Systems, German Aerospace Center, Robert-Hooke-Str. 7, 28359 Bremen, Germany;2. Institute of Planetary Research, German Aerospace Center, Rutherford str. 7, Berlin, Germany;1. Department of Mechanical Science and Engineering, Graduate School of Engineering, Nagoya University, Japan;2. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Japan |
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| Abstract: | The present state of knowledge of the structure of the atmospheres of Mars and Venus below 100 km is reviewed. Both atmospheres have been characterized to a remarkable degree, considering their remoteness from Earth. Mars' atmosphere is more variable, and less well defined. The variability is seasonal, diurnal, and latitude dependent, and also is strongly affected by atmospheric dust. Venus' atmosphere is less variable and better defined, as a result of numerous spacecraft missions. Mars' atmosphere is generally statically stable from the surface to 100 km, and its temperatures are controlled by radiative transfer moderated by vertical flow. Venus' lower atmosphere is stratified, with stable layers predominating. Its temperatures also are controlled by radiation and vertical motion. Thermal tidal motions occur in both atmospheres at about the same pressure levels, with larger amplitudes at Venus, consistent with the larger solar input at Venus. |
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