The first ISO workshop on analytical spectroscopy with SWS, LWS, PHT-S and CAM-CVF

(Oct 6-8, 1997, Madrid, Spain)

next up previous
Next: References Up: ISO Home Page Previous: ISOPEAKS Agenda Page

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 $\mu$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 $\mu$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 $\mu$m) up to the lower stratosphere at the mbar level (in the CH4 emission at 7.7 $\mu$m) or even the upper stratosphere at the $\mu$bar level (in the CH4 emission at 3.3 $\mu$m, in the H3+ lines around 4 $\mu$m, and in the H2O lines around 40 $\mu$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 $\mu$m at the center and between 2.3 and 45 $\mu$m at the poles (R=1500), and the CAM-CVF images recorded between 2.3 and 11 $\mu$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.

next up previous
Next: References Up: ISO Home Page Previous: ISOPEAKS Agenda Page

Postscript version