from the interior of the planet, which determines the kind of atmospheric dynamics that occur. Information about
The vertical structure of Jupiter's atmosphere is examined to better characterize the latitudinal region of the Galileo probe how radiation travels through Jupiter is important for the entry site: Ψ5Ψ-10Ψ planetographic latitude. One-hundred Hubdevelopment of models of solar system formation, planeble Space Telescope images of Jupiter taken with the 893-and tary cooling, and radiative transport, all of which can help 953-nm filters on 13 and 17 February 1995, 5 October 1995, us infer the early history of our own planet. The vertical and 14 May 1996 are analyzed, and a two-cloud model of the structure of the jovian atmosphere is complex and timejovian atmosphere (D. M. Kuehn and R. F. Beebe 1993, Icarus variable. Remote sensing of the clouds, haze, and gases 101, 282-292) is used to interpret center-to-limb variations of that compose Jupiter's atmosphere is fundamental for debright plume heads and adjacent dark areas in the latitude veloping a comprehensive picture of the atmosphere's verregion Ψ2Ψ-10Ψ. For both the plume heads and dark areas, the tical structure. top of the ammonia cloud deck reaches a pressure level of Over the past several decades, low and high phase angle roughly 200 mbar, and the cloud has an optical depth of between spacecraft observations of Jupiter along with high quality 6 and 7. The optical depth of the stratospheric haze layer is 0.59 for the plumes and 0.34 for the dark regions, while the ground-based imaging in methane absorption and continsingle scattering albedo of the ammonia cloud deck is 0.996 uum bands have enabled investigators to develop models for the plumes and 0.950 for the dark regions. Sensitivity tests for the vertical structure of the jovian atmosphere. West's motivated by the preliminary results from the Galileo probe (1979) analysis of ground-based imaging in three methane/ net flux radiometer and nephelometer experiments indicate that continuum filter pairs showed that the vertical structure of the ammonia cloud deck may have a patchy structure. Β© 1997 the South Tropical Zone (Οͺ21.7Π to Οͺ25.0Π planetographic Academic Press latitude) and the southern portion of the South Equatorial Belt (Οͺ15.6Π to Οͺ18.8Π) was better fit with a two-cloud model than with a diffuse reflecting-scattering model that mbar).