Modeling the Plasma Convection in Saturn's Inner Magnetosphere

Simple item page
dc.contributor.advisorHill, Thomas W.en_US
dc.contributor.committeeMemberToffoletto, Frank R.en_US
dc.contributor.committeeMemberLenardic, Adrianen_US
dc.creatorLiu, Xinen_US
dc.date.accessioned2013-09-16T15:51:46Zen_US
dc.date.accessioned2013-09-16T15:52:12Zen_US
dc.date.available2013-09-16T15:51:46Zen_US
dc.date.available2013-09-16T15:52:12Zen_US
dc.date.created2013-05en_US
dc.date.issued2013-09-16en_US
dc.date.submittedMay 2013en_US
dc.date.updated2013-09-16T15:52:12Zen_US
dc.description.abstractSaturn's magnetosphere is unique in the solar system. The rotation-driven convection consists of alternating channels of cool plasma from an interior source moving outward and hot plasma from outside moving inward, making Saturn’s inner magnetosphere a dynamical region. This thesis describes work on developing numerical models to simulate the plasma convection pattern in Saturn's inner magnetosphere. Chapter 2 introduces the numerical Rice Convection Model (RCM), a multi-fluid model that was originally developed for Earth’s magnetosphere. We adapt it for Saturn’s conditions in this thesis. In Chapter 3, we show results of initial RCM simulation runs, in which only cool plasma from the interior source is considered. We also include the Coriolis force and the pickup effect. Because the cool plasma is much denser than the hot plasma and always dominant in determining the convection pattern, it is important and necessary to investigate it first. Chapter 4 compares several cool plasma source models and determines the one that produces the best simulation results when compared to Cassini spacecraft observations. In Chapter 5, we add the finite temperature and associated plasma pressure of the cool plasma. The effect of ionospheric Pedersen conductance is also investigated. Finally in Chapter 6, we add hot plasma at the outer boundary, and simulate the V-shape signatures of the injection-dispersion events, which are considered the most definitive evidence of rotation-driven convection in Saturn's inner magnetosphere. Our simulations conform to the observed fact that wider, slower outflow channels of cooler, denser plasma alternate with narrower, faster inflow channels of hotter, more tenuous plasma. Comparisons between simulated and observed results show great consistency.en_US
dc.format.mimetypeapplication/pdfen_US
dc.identifier.citationLiu, Xin. "Modeling the Plasma Convection in Saturn's Inner Magnetosphere." (2013) Diss., Rice University. <a href="https://hdl.handle.net/1911/71990">https://hdl.handle.net/1911/71990</a>.en_US
dc.identifier.slug123456789/ETD-2013-05-425en_US
dc.identifier.urihttps://hdl.handle.net/1911/71990en_US
dc.language.isoengen_US
dc.rightsCopyright is held by the author, unless otherwise indicated. Permission to reuse, publish, or reproduce the work beyond the bounds of fair use or other exemptions to copyright law must be obtained from the copyright holder.en_US
dc.subjectMagnetosphereen_US
dc.subjectSaturnen_US
dc.subjectRCMen_US
dc.subjectConvectionen_US
dc.subjectPlasmaen_US
dc.subjectModelingen_US
dc.subjectSpace physicsen_US
dc.titleModeling the Plasma Convection in Saturn's Inner Magnetosphereen_US
dc.typeThesisen_US
dc.type.materialTexten_US
thesis.degree.departmentPhysics and Astronomyen_US
thesis.degree.disciplineNatural Sciencesen_US
thesis.degree.grantorRice Universityen_US
thesis.degree.levelDoctoralen_US
thesis.degree.nameDoctor of Philosophyen_US
Files
Original bundle
Now showing 1 - 1 of 1
Thumbnail Image
Name:
LIU-THESIS.pdf
Size:
34.36 MB
Format:
Adobe Portable Document Format
Download
License bundle
Now showing 1 - 1 of 1
No Thumbnail Available
Name:
license.txt
Size:
1.61 KB
Format:
Item-specific license agreed upon to submission
Description:
Download
Collections
Rice University Theses and Dissertations