Computer Science
Scientific paper
Feb 1999
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999icar..137..315r&link_type=abstract
Icarus, Volume 137, Issue Icarus, pp. 315-340.
Computer Science
14
Scientific paper
The 5-μm window in the spectrum of Jupiter is one of the few regions that gives access to the vertical structure of the troposphere between pressure levels of approximately 4 and 8 bar. Voyager-IRIS spectra obtained in 1979 during the Voyager flybys have been analyzed intensively over the past two decades. Most of these analyses concluded on a vertical cloud structure consisting of three layers: an ammonia cloud layer with a base around 0.5 bar, an ammonium-hydrosulfide layer at about 2 bar, and a water cloud layer with a base somewhere between 5 and 7 bar. However, the recent Galileo entry probe measurements of the vertical atmospheric structure in a hot spot region show a quite different picture. The data indicate only two cloud layers, at about 0.7 bar and 1.34 bar, and no significant cloud opacity between 2 and 22 bar, where the Probe measurements ended. New data from the Galileo-NIMS and ISO-SWS experiments agree with the Probe findings. The inclusion of cloud opacity between 5 and 7 bar in the model atmosphere results in a poor fit to the NIMS and ISO data. A comparison between Voyager-IRIS spectra and the ISO-SWS and Galileo-NIMS spectra shows a slope in the continuum level of the IRIS spectra for wavelengths shorter than 5 mum, not present in either SWS spectrum or the NIMS spectra. We show that to fit the IRIS spectra, an additional opacity somewhere between 3 and 8 bar is needed in the model atmosphere. We suggest that, most likely, a calibration problem occurred with the Voyager-IRIS data in this spectral region, even though temporal variations in the deep atmospheric structure of Jupiter cannot be ruled out altogether.
Carlson Richard W.
Drossart Pierre
Encrenaz Th.
Leader Frank
Roos-Serote Maarten
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