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A Study of the Jovian Atmospheric Structure using SWS and CAM-CVF
Th. Encrenaz 1 - E. Lellouch 1 - P. Drossart 1 - H. Feuchtgruber 2 - Th. de Graauw 3 - B. Altieri 2 - F. Lacombe 1 - D. Rouan 1 - D. Tiphène 1
1 DESPA, Observatoire de Paris, Meudon, France -2 ISO Science Operation Center, Villafranca, Spain -
3 SRON, Groningen, the Netherlands
The spectrum of Jupiter between 2.5 and 45 
m extends over a very
large dynamical range (100 000). It is characterized by a
reflected solar component which dominates at short wavelengths and a thermal
component which strongly increases beyond 4 m. The solar component
gives access to the albedo and the altitude of the NH3 cloud around 0.5 bar.
The thermal radiation probes different altitude ranges, from the deep
troposphere at several bars (at 5 m) up to the lower stratosphere
at the mbar level (in the CH4 emission at 7.7 m) or even
the upper stratosphere at the bar level (in the CH4 emission
at 3.3 m, in the H3+ lines around 4 m, and in the H2O lines
around 40 m).
We are using two sets of ISO data to retrieve the Jovian atmospheric structure
and its spatial variations: the SWS grating spectra, recorded
between 2.3 and 16.5 m at the center
and between 2.3 and 45 m at the poles (R=1500), and the CAM-CVF
images recorded between 2.3 and 11 m (R=50).
The comparison of the 3 SWS spectra should provide information on the
latitudinal variations of the thermal
stratospheric profile, from the analysis of the CH4 emission bands
(Encrenaz et al, 1996), and on the vertical distributions of several species:
NH3, PH3, hydrocarbons - including the recently detected CH3C2H -
and possibly stratospheric H2O (Feuchtgruber et al, 1997)
and CO2 (Lellouch et al, 1997). The CAM-CVF images provide a new information
about the spatial structure of the NH3 cloud and the temperature field
in the lower stratosphere. The reduction of these data is in progress.
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Postscript version