Article ID | Journal | Published Year | Pages | File Type |
---|---|---|---|---|
1773190 | Icarus | 2013 | 18 Pages |
Abstract
Using high-resolution Cassini ISS images with wavelengths ranging from the ultraviolet to the near infrared, we have retrieved Saturn's atmospheric aerosol structure and properties for a broad range of latitudes in the southern hemisphere. The observations are consistent with two distinct layers of haze above a scattered cloud. Each layer is characterized by a vertical location, an optical thickness, and an effective mean particle size, all of which vary with latitude. The tropospheric haze is optically thickest and extends to the greatest heights (â¼40 mbar) over the equator; its top surface is at significantly greater depths (â¼150 mbar) at mid-latitudes. The height of the haze correlates well with position of the tropopause as indicated by the temperature field. Beneath this haze, we find a scattered denser cloud responsible for small-scale contrasts at an average depth of 1.75 ± 0.4 bar, with some features as deep as 2.5 bar or greater.
Related Topics
Physical Sciences and Engineering
Earth and Planetary Sciences
Space and Planetary Science
Authors
Michael T. Roman, Don Banfield, Peter J. Gierasch,