Saturn'S Cloud Structure Inferred From Cassini Iss
| dc.contributor.author | Roman, Michael | en_US |
| dc.contributor.chair | Gierasch, Peter Jay | en_US |
| dc.contributor.committeeMember | Veverka, Joseph Frank | en_US |
| dc.contributor.committeeMember | Hess, Peter George Mueller | en_US |
| dc.contributor.committeeMember | Banfield, Donald J | en_US |
| dc.date.accessioned | 2013-02-22T14:16:16Z | |
| dc.date.available | 2017-09-26T06:00:49Z | |
| dc.date.issued | 2012-05-27 | en_US |
| dc.description.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. Each layer is characterized by a vertical location, an optical depth, and a mean particle size, all of which vary with latitude. The tropospheric haze is optically thickest and extends to the greatest heights (~40 mbar) over the equator; its top surface is at significantly greater depths (~150 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 deeper than 2.5 bar. | en_US |
| dc.identifier.other | bibid: 8251357 | |
| dc.identifier.uri | https://hdl.handle.net/1813/31468 | |
| dc.language.iso | en_US | en_US |
| dc.subject | Saturns Atmosphere | en_US |
| dc.subject | Vertical Structure | en_US |
| dc.subject | Clouds and Haze | en_US |
| dc.title | Saturn'S Cloud Structure Inferred From Cassini Iss | en_US |
| dc.type | dissertation or thesis | en_US |
| thesis.degree.discipline | Atmospheric Science | |
| thesis.degree.grantor | Cornell University | en_US |
| thesis.degree.level | Master of Science | |
| thesis.degree.name | M.S., Atmospheric Science |
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