Persistent Link:
http://hdl.handle.net/10150/193360
Title:
Viscous Relaxation of Craters on Enceladus
Author:
Smith, Diana Elizabeth
Issue Date:
2008
Publisher:
The University of Arizona.
Rights:
Copyright © 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.
Abstract:
Cassini spacecraft images of Enceladus' surface have revealed diverse terrains---some heavily cratered, others almost devoid of craters, and even some with ridges and fractures. We have documented crater morphologies in regions for which high-resolution data are available (140 to 360 W and 90 S to 60 N). The south polar region shows a dearth of craters, in sharp contrast to the heavily cratered northern latitudes. Tectonized regions such as Sarandib and Diyar Planitiae also have low crater densities. Viscously relaxed craters are found in the apparently young regions of the anti-Saturnian and trailing hemispheres, as well as in the older, upper northern latitudes. By modeling the viscoelastic relaxation of craters on Enceladus using TEKTON, a finite-element code, we predict large geographical variation in heat flow and a complicated thermal history on Enceladus. Our results are consistent with the planitiae being older examples of the South Polar Terrain, supporting a satellite-reorientation hypothesis.
Type:
text; Electronic Thesis
Keywords:
Planetary Science; Enceladus; Tectonics; Impact Craters
Degree Name:
MS
Degree Level:
masters
Degree Program:
Planetary Sciences; Graduate College
Degree Grantor:
University of Arizona
Advisor:
Melosh, Henry J.
Committee Chair:
Melosh, Henry J.

Full metadata record

DC FieldValue Language
dc.language.isoENen_US
dc.titleViscous Relaxation of Craters on Enceladusen_US
dc.creatorSmith, Diana Elizabethen_US
dc.contributor.authorSmith, Diana Elizabethen_US
dc.date.issued2008en_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.description.abstractCassini spacecraft images of Enceladus' surface have revealed diverse terrains---some heavily cratered, others almost devoid of craters, and even some with ridges and fractures. We have documented crater morphologies in regions for which high-resolution data are available (140 to 360 W and 90 S to 60 N). The south polar region shows a dearth of craters, in sharp contrast to the heavily cratered northern latitudes. Tectonized regions such as Sarandib and Diyar Planitiae also have low crater densities. Viscously relaxed craters are found in the apparently young regions of the anti-Saturnian and trailing hemispheres, as well as in the older, upper northern latitudes. By modeling the viscoelastic relaxation of craters on Enceladus using TEKTON, a finite-element code, we predict large geographical variation in heat flow and a complicated thermal history on Enceladus. Our results are consistent with the planitiae being older examples of the South Polar Terrain, supporting a satellite-reorientation hypothesis.en_US
dc.typetexten_US
dc.typeElectronic Thesisen_US
dc.subjectPlanetary Scienceen_US
dc.subjectEnceladusen_US
dc.subjectTectonicsen_US
dc.subjectImpact Cratersen_US
thesis.degree.nameMSen_US
thesis.degree.levelmastersen_US
thesis.degree.disciplinePlanetary Sciencesen_US
thesis.degree.disciplineGraduate Collegeen_US
thesis.degree.grantorUniversity of Arizonaen_US
dc.contributor.advisorMelosh, Henry J.en_US
dc.contributor.chairMelosh, Henry J.en_US
dc.contributor.committeememberShowman, Adamen_US
dc.identifier.proquest2759en_US
dc.identifier.oclc659749792en_US
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