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Available online at www.sciencedirect.com Planetary and Space Science 52 (2004) 397414
 

Summary: Available online at www.sciencedirect.com
Planetary and Space Science 52 (2004) 397­414
www.elsevier.com/locate/pss
On the water abundance in the atmosphere of Jupiter
M. Roos-Serotea;, S.K. Atreyab, M.K. Wongc, P. Drossartd
aLisbon Astronomical Observatory, Tapada da Ajuda, 1349-018 Lisbon, Portugal
bDepartment of Atmospheric, Oceanic and Space Sciences, University of Michigan, Ann Arbor, MI 48109-2143, USA
cNASA/Goddard Space Flight Center, USA
dObservatory of Paris at Meudon, 5 Place J. Janssen, 92195 Meudon Cedex, France
Received 20 January 2003; accepted 16 June 2003
Abstract
In this paper, we attempt to place constraints on the possible global abundance of water and the average vertical cloud structure in the
atmosphere of Jupiter. Based on the analysis of the Galileo Near-Infrared Mapping Spectrometer data, we ˙nd that in the atmosphere of
Jupiter down to 6­8 bar, particularly in the North Equatorial Belt (NEB) region, the overall O/H ratio is compatible with one or more
times the solar value of this ratio. We also ˙nd that if water clouds form at the levels where they are expected from thermochemical
equilibrium calculations for a given deep O/H ratio, then subsolar values of the O/H ratio cannot be reconciled with the analyzed data.
However, these results are dependent on the model atmosphere, in particular the detailed vertical distribution of cloud opacity. Therefore,
they should be considered with care, until new observations on the vertical cloud structure become available. The water vapor mixing
ratio in the NEB displays large spatial variations. The same set of data yield subsaturated mixing ratios of ammonia to atmospheric levels
of about 4 bar. This depletion of ammonia to great depths, as seen by the Galileo Probe in the hot spot where it entered, appears to be a

  

Source: Atreya, Sushil - Department of Atmospheric, Oceanic and Space Science, University of Michigan

 

Collections: Physics