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    Solar magnetic fields: source, evolution, and interaction with planetary magnetospheres

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    Burkholder_B_2019.pdf
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    Author
    Burkholder, Brandon
    Chair
    Delamere, Peter
    Committee
    Otto, Antonius
    Newman, David
    Ng, Chung-Sang
    Connor, Hyunju
    Keyword
    solar magnetic fields
    planets
    magnetospheres
    heliosphere
    astrophysics
    sun
    corona
    magnetic fields
    solar wind
    Metadata
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    URI
    http://hdl.handle.net/11122/10611
    Abstract
    Magnetized 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.
    Description
    Dissertation (Ph.D.) University of Alaska Fairbanks, 2019
    Table of Contents
    1. 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.
    Date
    2019-08
    Type
    Dissertation
    Collections
    Physics

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