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dc.contributor.advisorHolberg, Jay B.en_US
dc.contributor.authorSepahi, Mohammad Mehdi, 1962-
dc.creatorSepahi, Mohammad Mehdi, 1962-en_US
dc.date.accessioned2013-05-16T09:52:27Z
dc.date.available2013-05-16T09:52:27Z
dc.date.issued1992en_US
dc.identifier.urihttp://hdl.handle.net/10150/292044
dc.description.abstractWe conducted a detailed study and comparative analysis of the Voyager UVS and PPS stellar occultations of the Uranian ring system. The primary objective of this study was the determination of the constraints on the sizes of the ring particles. The Voyager UVS and PPS occultations probed the epsilon and delta rings at significantly shorter wavelengths (0.11 μm and 0.27 μm, respectively) and at substantially different viewing geometries than a large number of existing Earth-based occultations. These differences combine to produce a unique mutual sensitivity among the UVS, PPS and Earth-based observations to the particle properties of the rings. Our results yield slight, but significant differences between PPS and UVS optical depths. We interpret these differences as wavelength dependent scattering due to a population of small particles in the mm to cm size range in epsilon and delta rings. The size distribution of particles in epsilon and delta rings were found to be similar, the main difference being the total number of particles. In contrast to studies at longer wavelengths, our results imply a relatively steep particle size distribution characterized by a power law of index 3 or greater.
dc.language.isoen_USen_US
dc.publisherThe University of Arizona.en_US
dc.rightsCopyright © is held by the author. Digital access to this material is made possible by the University Libraries, University of Arizona. Further transmission, reproduction or presentation (such as public display or performance) of protected items is prohibited except with permission of the author.en_US
dc.subjectPhysics, Astronomy and Astrophysics.en_US
dc.subjectPhysics, Optics.en_US
dc.titleVoyager 2 stellar occultation probe of the Uranian rings: A detailed comparison of UVS and PPS resultsen_US
dc.typetexten_US
dc.typeThesis-Reproduction (electronic)en_US
thesis.degree.grantorUniversity of Arizonaen_US
thesis.degree.levelmastersen_US
dc.identifier.proquest1351334en_US
thesis.degree.disciplineGraduate Collegeen_US
thesis.degree.disciplinePhysicsen_US
thesis.degree.nameM.S.en_US
dc.identifier.bibrecord.b27149407en_US
refterms.dateFOA2018-06-16T04:57:16Z
html.description.abstractWe conducted a detailed study and comparative analysis of the Voyager UVS and PPS stellar occultations of the Uranian ring system. The primary objective of this study was the determination of the constraints on the sizes of the ring particles. The Voyager UVS and PPS occultations probed the epsilon and delta rings at significantly shorter wavelengths (0.11 μm and 0.27 μm, respectively) and at substantially different viewing geometries than a large number of existing Earth-based occultations. These differences combine to produce a unique mutual sensitivity among the UVS, PPS and Earth-based observations to the particle properties of the rings. Our results yield slight, but significant differences between PPS and UVS optical depths. We interpret these differences as wavelength dependent scattering due to a population of small particles in the mm to cm size range in epsilon and delta rings. The size distribution of particles in epsilon and delta rings were found to be similar, the main difference being the total number of particles. In contrast to studies at longer wavelengths, our results imply a relatively steep particle size distribution characterized by a power law of index 3 or greater.


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