Time Evolution of Pulsar Magnetosphere: An Implicit Approach

dc.contributor.advisorSchlegel, Eric
dc.contributor.authorSreekumar, Sushilkumar
dc.contributor.committeeMemberSpeck, Angela
dc.contributor.committeeMemberLopez-Mobilia, Rafael
dc.contributor.committeeMemberChen, Liao
dc.contributor.committeeMemberPannuti, Thomas
dc.creator.orcidhttps://orcid.org/0000-0001-9617-5902
dc.date.accessioned2024-01-26T23:09:00Z
dc.date.available2024-01-26T23:09:00Z
dc.date.issued2020
dc.descriptionThe author has granted permission for their work to be available to the general public.
dc.description.abstractWe apply a computationally efficient technique to validate the global structure of the pulsarmagnetosphere. This is achieved by implementing a three dimensional, computationally intense,implicit Crank-Nicolson finite-difference scheme. We are particularly interested in the magneti-cally dominated region around a neutron star. This region of magnetic influence, called the mag-netosphere is evolved under the approximation of force-free electrodynamics (FFE). The mainobjective of this dissertation is to present our code and use it to demonstrate and verify the nowwidely accepted global features of a pulsar magnetosphere. Our implicit approach is tested for thetwo extreme conditions of the magnetosphere: vacuum and FFE. Our results qualitatively agreewith previously developed time-dependent models for an oblique rotator. The current density cor-responding to the FF approximation is first evolved using the advection/perpendicular term andthen by allowing a non-zero parallel component. We also demonstrate, in line with previous stud-ies, that our simulations can run steadily for several stellar rotations. Further study is howeverrequired to understand the structure of the magnetosphere when a non-zero parallel componentof the current density is incorporated. With better spatial and time resolution implementing animplicit method is important as the approach can be treated efficiently towards dissipative termswithin a current density equation. In addition, the approach can be useful to investigate magneto-spheres filled with resistive plasma, achieve better resolution current sheets and in developing anefficient Particle-In-Cell (PIC) technique.
dc.description.departmentPhysics and Astronomy
dc.format.extent105 pages
dc.format.mimetypeapplication/pdf
dc.identifier.isbn9798557049665
dc.identifier.urihttps://hdl.handle.net/20.500.12588/2725
dc.languageen
dc.subjectComputational
dc.subjectCrank-Nicolson
dc.subjectMagnetosphere
dc.subjectNeutron Star
dc.subjectPulsar
dc.subject.classificationPhysics
dc.subject.classificationAstrophysics
dc.titleTime Evolution of Pulsar Magnetosphere: An Implicit Approach
dc.typeThesis
dc.type.dcmiText
dcterms.accessRightspq_OA
thesis.degree.departmentPhysics and Astronomy
thesis.degree.grantorUniversity of Texas at San Antonio
thesis.degree.levelDoctoral
thesis.degree.nameDoctor of Philosophy

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