{"id":{"repo_id":"uiuc","oai_identifier":"oai:www.ideals.illinois.edu:2142/23908"},"canonical_url":"https://search.dev.ndltd.org/etd/uiuc/oai:www.ideals.illinois.edu:2142/23908","repository":{"repo_id":"uiuc","name":"University of Illinois - Urbana-Champaign","base_url":"https://www.ideals.illinois.edu/oai-pmh"},"display":{"title":"Magnetospheres of neutron stars accreting from disks","abstract":"This thesis presents quantitative models of the magnetosphere of a magnetic star surrounded by a thin plasma disk. The model is motivated by the currently accepted picture of many accretion-powered pulsars as strongly magnetic neutron stars accreting from disks. It may also be relevant to the luminous galactic bulge X-ray sources that display quasi-periodic oscillations in intensity. These QPO sources are thought by some to be weakly magnetic neutron stars accreting from disks. In constructing these magnetospheric models, I assume that the magnetic field is static and axisymmetric about the axis of the disk. I also assume that the magnetic field is in force-free equilibrium. The validity of these simplifying assumptions for astrophysical systems is discussed in some detail. The boundary conditions on the magnetic field at the disk have been chosen to mimic the expected electrodynamic interaction between a magnetic neutron star and an accretion disk. These boundary conditions cause the second-order partial differential equation for the magnetic flux function to be non-linear. This equation is solved iteratively using finite-difference techniques on a grid of points covering the volume of the magnetosphere. Solutions have been obtained for two different configurations. In one, the disk extends to the stellar surface while in the other, there is a gap between the inner edge of the disk and the surface of the star. The solutions determine the poloidal and toroidal components of the magnetic field as a function of position within the magnetosphere. From these components, I calculate the torque exerted on the star and the energy stored in the twisted magnetic field. The significance of these solutions for accretion-powered pulsars and QPO sources is briefly considered. Specifically, I discuss the likely effect of the electrodynamic interaction between the disk and the star on the structure of the magnetic field, especially near the disk's inner edge. I also discuss the maximum pitch and largest spin-up and spin-down torques that can be supported by the magnetic field.","abstract_html":"This thesis presents quantitative models of the magnetosphere of a magnetic star surrounded by a thin plasma disk. The model is motivated by the currently accepted picture of many accretion-powered pulsars as strongly magnetic neutron stars accreting from disks. It may also be relevant to the luminous galactic bulge X-ray sources that display quasi-periodic oscillations in intensity. These QPO sources are thought by some to be weakly magnetic neutron stars accreting from disks. In constructing these magnetospheric models, I assume that the magnetic field is static and axisymmetric about the axis of the disk. I also assume that the magnetic field is in force-free equilibrium. The validity of these simplifying assumptions for astrophysical systems is discussed in some detail. The boundary conditions on the magnetic field at the disk have been chosen to mimic the expected electrodynamic interaction between a magnetic neutron star and an accretion disk. These boundary conditions cause the second-order partial differential equation for the magnetic flux function to be non-linear. This equation is solved iteratively using finite-difference techniques on a grid of points covering the volume of the magnetosphere. Solutions have been obtained for two different configurations. In one, the disk extends to the stellar surface while in the other, there is a gap between the inner edge of the disk and the surface of the star. The solutions determine the poloidal and toroidal components of the magnetic field as a function of position within the magnetosphere. From these components, I calculate the torque exerted on the star and the energy stored in the twisted magnetic field. The significance of these solutions for accretion-powered pulsars and QPO sources is briefly considered. Specifically, I discuss the likely effect of the electrodynamic interaction between the disk and the star on the structure of the magnetic field, especially near the disk's inner edge. I also discuss the maximum pitch and largest spin-up and spin-down torques that can be supported by the magnetic field.","abstract_has_math":false,"creators":["Zylstra, Gregory Jay"],"institution":null,"degree_name":"Ph.D.","degree_level":"Dissertation","degree_discipline":"Physics","degree_department":null,"school":null,"contributors":["Lamb, Frederick K."],"advisors":[],"committee_chairs":[],"committee_members":[],"year":2011,"date_issued":"2011-05-17T14:58:35Z","date_published":"2011-05-17T14:58:35Z","updated_at":"2026-07-22T22:25:22Z","subjects":["magnetospheres","neutron stars","thin plasma disk","accretion-powered pulsars","quasi-periodic oscillations"],"languages":["en"],"rights":["1988 Gregory Jay Zylstra"],"rights_urls":[],"identifier_entries":[{"key":"dc:identifier","label":"Identifier","values":["3488454"],"render_values":[{"text":"3488454","href":null,"code":true}]}]},"links":{"outbound_url":"http://hdl.handle.net/2142/23908","outbound_label":"Handle","outbound_source":"dc:identifier"},"metadata_groups":[{"id":"people","label":"People","entries":[{"key":"dc:contributor","label":"Contributor","values":["Lamb, Frederick K."]},{"key":"dc:creator","label":"Author","values":["Zylstra, Gregory Jay"]}]},{"id":"academic_context","label":"Academic Context","entries":[{"key":"dc:date","label":"Dc Date","values":["2011-05-17T14:58:35Z","10000-01-01","1988"]},{"key":"dc:type","label":"Dc Type","values":["Dissertation / Thesis","text"]},{"key":"thesis:degree_discipline","label":"Discipline","values":["Physics"]},{"key":"thesis:degree_level","label":"Degree Level","values":["Dissertation"]},{"key":"thesis:degree_name","label":"Degree Name","values":["Ph.D."]}]},{"id":"subjects_keywords","label":"Subjects and Keywords","entries":[{"key":"dc:subject","label":"Dc Subject","values":["magnetospheres","neutron stars","thin plasma disk","accretion-powered pulsars","quasi-periodic oscillations"]}]},{"id":"language_rights","label":"Language and Rights","entries":[{"key":"dc:language","label":"Dc Language","values":["en"]},{"key":"dc:rights","label":"Dc Rights","values":["1988 Gregory Jay Zylstra"]}]},{"id":"identifiers","label":"Identifiers","entries":[{"key":"dc:identifier","label":"Identifier","values":["3488454","http://hdl.handle.net/2142/23908"]}]},{"id":"additional","label":"Additional Metadata","entries":[{"key":"dc:description","label":"Description","values":["This thesis presents quantitative models of the magnetosphere of a magnetic star surrounded by a thin plasma disk. The model is motivated by the currently accepted picture of many accretion-powered pulsars as strongly magnetic neutron stars accreting from disks. It may also be relevant to the luminous galactic bulge X-ray sources that display quasi-periodic oscillations in intensity. These QPO sources are thought by some to be weakly magnetic neutron stars accreting from disks. In constructing these magnetospheric models, I assume that the magnetic field is static and axisymmetric about the axis of the disk. I also assume that the magnetic field is in force-free equilibrium. The validity of these simplifying assumptions for astrophysical systems is discussed in some detail. The boundary conditions on the magnetic field at the disk have been chosen to mimic the expected electrodynamic interaction between a magnetic neutron star and an accretion disk. These boundary conditions cause the second-order partial differential equation for the magnetic flux function to be non-linear. This equation is solved iteratively using finite-difference techniques on a grid of points covering the volume of the magnetosphere. Solutions have been obtained for two different configurations. In one, the disk extends to the stellar surface while in the other, there is a gap between the inner edge of the disk and the surface of the star. The solutions determine the poloidal and toroidal components of the magnetic field as a function of position within the magnetosphere. From these components, I calculate the torque exerted on the star and the energy stored in the twisted magnetic field. The significance of these solutions for accretion-powered pulsars and QPO sources is briefly considered. Specifically, I discuss the likely effect of the electrodynamic interaction between the disk and the star on the structure of the magnetic field, especially near the disk's inner edge. I also discuss the maximum pitch and largest spin-up and spin-down torques that can be supported by the magnetic field.","Submitted by Carolyn Mead (cmead2@illinois.edu) on 2011-05-17T14:58:35Z No. of bitstreams: 1 1988_zylstra.pdf: 5859826 bytes, checksum: 5766ca687bd48ab1f5ff31bea35902e2 (MD5)","Made available in DSpace on 2011-05-17T14:58:35Z (GMT). No. of bitstreams: 1 1988_zylstra.pdf: 5859826 bytes, checksum: 5766ca687bd48ab1f5ff31bea35902e2 (MD5) Previous issue date: 1988","Item marked as restricted to the 'UIUC Users [automated]' Group (id=2) by Carolyn Mead (cmead2@illinois.edu) on 2011-05-17T14:58:35Z Item is restricted indefinitely.","Restriction data tranferred 2014-07-01T11:13:09-05:00 Original Data Group with Access UIUC Users [automated] Release Date: none Reason: Thesis","Thesis","U of I Only"]},{"key":"dc:title","label":"Title","values":["Magnetospheres of neutron stars accreting from disks"]}]}],"canonical_facts":{"dc:contributor":["Lamb, Frederick K."],"dc:creator":["Zylstra, Gregory Jay"],"dc:date":["2011-05-17T14:58:35Z","10000-01-01","1988"],"dc:description":["This thesis presents quantitative models of the magnetosphere of a magnetic star surrounded by a thin plasma disk. The model is motivated by the currently accepted picture of many accretion-powered pulsars as strongly magnetic neutron stars accreting from disks. It may also be relevant to the luminous galactic bulge X-ray sources that display quasi-periodic oscillations in intensity. These QPO sources are thought by some to be weakly magnetic neutron stars accreting from disks. In constructing these magnetospheric models, I assume that the magnetic field is static and axisymmetric about the axis of the disk. I also assume that the magnetic field is in force-free equilibrium. The validity of these simplifying assumptions for astrophysical systems is discussed in some detail. The boundary conditions on the magnetic field at the disk have been chosen to mimic the expected electrodynamic interaction between a magnetic neutron star and an accretion disk. These boundary conditions cause the second-order partial differential equation for the magnetic flux function to be non-linear. This equation is solved iteratively using finite-difference techniques on a grid of points covering the volume of the magnetosphere. Solutions have been obtained for two different configurations. In one, the disk extends to the stellar surface while in the other, there is a gap between the inner edge of the disk and the surface of the star. The solutions determine the poloidal and toroidal components of the magnetic field as a function of position within the magnetosphere. From these components, I calculate the torque exerted on the star and the energy stored in the twisted magnetic field. The significance of these solutions for accretion-powered pulsars and QPO sources is briefly considered. Specifically, I discuss the likely effect of the electrodynamic interaction between the disk and the star on the structure of the magnetic field, especially near the disk's inner edge. I also discuss the maximum pitch and largest spin-up and spin-down torques that can be supported by the magnetic field.","Submitted by Carolyn Mead (cmead2@illinois.edu) on 2011-05-17T14:58:35Z No. of bitstreams: 1 1988_zylstra.pdf: 5859826 bytes, checksum: 5766ca687bd48ab1f5ff31bea35902e2 (MD5)","Made available in DSpace on 2011-05-17T14:58:35Z (GMT). No. of bitstreams: 1 1988_zylstra.pdf: 5859826 bytes, checksum: 5766ca687bd48ab1f5ff31bea35902e2 (MD5) Previous issue date: 1988","Item marked as restricted to the 'UIUC Users [automated]' Group (id=2) by Carolyn Mead (cmead2@illinois.edu) on 2011-05-17T14:58:35Z Item is restricted indefinitely.","Restriction data tranferred 2014-07-01T11:13:09-05:00 Original Data Group with Access UIUC Users [automated] Release Date: none Reason: Thesis","Thesis","U of I Only"],"dc:identifier":["3488454","http://hdl.handle.net/2142/23908"],"dc:language":["en"],"dc:rights":["1988 Gregory Jay Zylstra"],"dc:subject":["magnetospheres","neutron stars","thin plasma disk","accretion-powered pulsars","quasi-periodic oscillations"],"dc:title":["Magnetospheres of neutron stars accreting from disks"],"dc:type":["Dissertation / Thesis","text"],"thesis:degree_discipline":["Physics"],"thesis:degree_level":["Dissertation"],"thesis:degree_name":["Ph.D."]},"updated_at":"2026-07-22T22:25:22Z"}