Atmospheric Circulation and Dynamics

  • Sanjay S. LimayeEmail author
  • Miriam Rengel
Part of the ISSI Scientific Report Series book series (ISSI, volume 11)


The deep atmosphere of Venus ( ∼ 180 km including the thermosphere) presents both observational and modeling challenges. Its thick, nearly uniform global cloud cover makes it difficult to fathom the vertical structure of the global circulation through available techniques that are applied to Earth’s atmosphere. Further, the slow rotation of the planet and the consequential prevailing cyclostrophic balance restricts easy inferences about the meridional flow and circulation (Gierasch et al. 1997, Read 1986, Schubert et al. 2007).


Zonal Wind Radio Occultation Meridional Flow Night Side Venus Express 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.


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Copyright information

© Springer Science+Business Media New York 2013

Authors and Affiliations

  1. 1.Space Science and Engineering CenterUniversity of WisconsinWisconsinUSA
  2. 2.Max-Planck-Institut fur SonnensystemforschungLindauGermany

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