The thermal structure of the Venus atmosphere: Intercomparison of Venus Express and ground based observations of vertical temperature and density profiles
Journal
Date Issued
2017
Author(s)
Limaye, Sanjay S.
•
Lebonnois, Sebastien
•
Mahieux, Arnaud
•
Pätzold, Martin
•
Bougher, Steven
•
Bruinsma, Sean
•
Chamberlain, Sarah
•
Clancy, R. Todd
•
Gérard, Jean-Claude
•
Gilli, Gabriella
•
•
Haus, Rainer
•
Herrmann, Maren
•
Imamura, Takeshi
•
Kohler, Erika
•
Krause, Pia
•
•
Montmessin, Franck
•
Pere, Christophe
•
Persson, Moa
•
Piccialli, Arianna
•
Rengel, Miriam
•
Rodin, Alexander
•
Sandor, Brad
•
Sornig, Manuela
•
Svedhem, Håkan
•
Tellmann, Silvia
•
Tanga, Paolo
•
Vandaele, Ann C.
•
Widemann, Thomas
•
Wilson, Colin F.
•
Müller-Wodarg, Ingo
•
Zasova, Ludmila
Abstract
The Venus International Reference Atmosphere (VIRA) model contains tabulated values of temperature and number densities obtained by the experiments on the Venera entry probes, Pioneer Venus Orbiter and multi-probe missions in the 1980s. The instruments on the recent Venus Express orbiter mission generated a significant amount of new observational data on the vertical and horizontal structure of the Venus atmosphere from 40 km to about 180 km altitude from April 2006 to November 2014. Many ground based experiments have provided data on the upper atmosphere (90-130 km) temperature structure since the publication of VIRA in 1985. The "Thermal Structure of the Venus Atmosphere" Team was supported by the International Space Studies Institute (ISSI), Bern, Switzerland, from 2013 to 2015 in order to combine and compare the ground-based observations and the VEx observations of the thermal structure as a first step towards generating an updated VIRA model. Results of this comparison are presented in five latitude bins and three local time bins by assuming hemispheric symmetry. The intercomparison of the ground-based and VEx results provides for the first time a consistent picture of the temperature and density structure in the 40 km-180 km altitude range. The Venus Express observations have considerably increased our knowledge of the Venus atmospheric thermal structure above ∼40 km and provided new information above 100 km. There are, however, still observational gaps in latitude and local time above certain regions. Considerable variability in the temperatures and densities is seen above 100 km but certain features appear to be systematically present, such as a succession of warm and cool layers. Preliminary modeling studies support the existence of such layers in agreement with a global scale circulation. The intercomparison focuses on average profiles but some VEx experiments provide sufficient global coverage to identify solar thermal tidal components.
Volume
294
Start page
124
Issn Identifier
0019-1035
Ads BibCode
2017Icar..294..124L
Rights
open.access
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