one to track the winds while they also limit the contrast one sees on the planet. We have determined the distribution of Photometrically calibrated grism spectra of Jupiter in the H (1.45-1.8 m) and K (1.95-2.5 m) bands with a resolution aerosols in Jupiter's upper trophosphere and lower stratoof about 100 were taken with the 5-m Hale telescope at Palomar sphere using near-infrared reflection spectra. We have also in August of 1995. The spectra were obtained as meridional begun to make inferences about particle mechanics above cuts at six different longitudes on the planet, with one cut the visible cloud deck from these vertical and meridional crossing the Great Red Spot.
distributions of aerosols.
The
technique outlined in D. Banfield et al. (1996, Icarus A good review of the state of knowledge of the cloud 121, 389-410) for the retrieval of scatterer density with altitude layers on Jupiter was given by West et al. (1986). They from near-infrared spectra is used and refined. It is expected presented a broad picture of the results of theoretical prethat this retrieval technique will find use in the interpretation dictions and observational measurements of the spatial of many atmospheric near-infrared reflection spectra, especially distribution of jovian aerosols. Lewis (1969a,b) and those from Galileo NIMS and Cassini VIMS. For the wavelengths and spectral resolution used in this study, the sensitivity Weidenschilling and Lewis (1973) predicted condensate of the inversions extends from pressure levels near 400 mbar clouds in the troposphere of H 2 O-NH 3 , perhaps NH 4 SH up to about 20 mbar. Employing this inversion technique on and NH 3 at and above pressures of 6, 2, and 0.7 bars, the spectra yields well-resolved jovian cloud densities for Շ respectively. Strobel (1983) reviewed the photochemistry 0.1, as a function of latitude and altitude. of Jupiter and discussed predictions of the formation of The density of scatterers is minimum at a height where the N 2 H 4 at a pressure of about 100 mbar. This N 2 H 4 would pressure is about 100 mbar and increases both upward and condense at stratospheric temperatures, forming a high downward from this level. The minimum near 100 mbar can altitude haze layer. Pryor and Hord (1991) suggested that be explained by coagulation of settling particles, leading to an hydrocarbons formed through auroral processes might creincrease in fall speed. The results indicate that stratospheric haze particles are generated at heights where p Շ 20 ate aerosols even higher in the polar stratosphere.
mbar.