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dc.contributor.authorBurkholder, Brandon
dc.date.accessioned2019-10-10T18:05:05Z
dc.date.available2019-10-10T18:05:05Z
dc.date.issued2019-08
dc.identifier.urihttp://hdl.handle.net/11122/10611
dc.descriptionDissertation (Ph.D.) University of Alaska Fairbanks, 2019en_US
dc.description.abstractMagnetized plasmas with twisted and filamented magnetic fields are pervasive throughout the heliosphere. In the solar magnetic field, photospheric convection on scale sizes from granules to differential rotation is responsible for driven magnetic reconnection. These reconnection sites are closely related to the magnetic topology, which is highly complex as the magnetic field is structured by a network of many thousands of magnetic flux concentrations. The coronal plasma overlying this "magnetic carpet" is the source of the solar wind flow, which has been found to be turbulent as close to the sun as our observations can currently resolve. At 1 AU, observations have also revealed a highly structured solar wind which we posit in this thesis originates in the corona rather than forming in-transit. Further, the solar wind-magnetosphere interaction depends on variability in the solar wind. When the boundary between solar wind plasma and magnetospheric plasma is unstable to the growth of Kelvin-Helmholtz waves, driven magnetic reconnection can occur on the magnetopause boundary. Such reconnection allows magnetic field to thread the boundary and transport can take place. We quantify the solar wind interaction for a corotation dominated system in terms of the mass and momentum transport driven by Kelvin-Helmholtz instabilities. Model-data comparisons are performed in this thesis using both the magnetohydrodynamic and hybrid-kinetic approaches for fluid simulations.en_US
dc.description.tableofcontents1. Introduction - 2. Magnetic connectivity in the corona as a source of solar wind structure - 3. Magnetic reconnection of solar flux tubes and coronal reconnection signatures in the solar wind at 1 AU - 4. Kelvin Helmholtz at Saturn - 5. Summary and future work -- Appendices -- Bibliography.en_US
dc.language.isoen_USen_US
dc.subjectsolar magnetic fieldsen_US
dc.subjectplanetsen_US
dc.subjectmagnetospheresen_US
dc.subjectheliosphereen_US
dc.subjectastrophysicsen_US
dc.subjectsunen_US
dc.subjectcoronaen_US
dc.subjectmagnetic fieldsen_US
dc.subjectsolar winden_US
dc.titleSolar magnetic fields: source, evolution, and interaction with planetary magnetospheresen_US
dc.typeDissertationen_US
dc.type.degreephden_US
dc.identifier.departmentDepartment of Physicsen_US
dc.contributor.chairDelamere, Peter
dc.contributor.committeeOtto, Antonius
dc.contributor.committeeNewman, David
dc.contributor.committeeNg, Chung-Sang
dc.contributor.committeeConnor, Hyunju
refterms.dateFOA2020-03-07T01:23:36Z


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