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dc.contributor.advisorBenz, Willyen_US
dc.contributor.authorFryer, Christopher Lee, 1969-
dc.creatorFryer, Christopher Lee, 1969-en_US
dc.date.accessioned2013-08-15T10:13:49Z
dc.date.available2013-08-15T10:13:49Z
dc.date.issued1996en_US
dc.identifier.urihttp://hdl.handle.net/10150/298809
dc.description.abstractThis dissertation clarifies two aspects of neutron-star formation and evolution: the formation of neutron stars through the accretion-induced collapse of white dwarfs and the common envelope evolution of neutron stars. In both cases, we utilize a 1-D lagrangean and 2-D SPH hydrodynamics codes equipped with a broad range of physics including neutrino emission, absorption, and transport, general relativity and dense equations of state. These results are then applied to a Monte-Carlo population synthesis code to study the effects of kicks placed upon neutron stars near the time of their formation. By comparing these results with the current observational data, we find that a bimodal kick distribution of neutron-star kicks is required.
dc.language.isoen_USen_US
dc.publisherThe University of Arizona.en_US
dc.rightsCopyright © is held by the author. Digital access to this material is made possible by the University Libraries, University of Arizona. Further transmission, reproduction or presentation (such as public display or performance) of protected items is prohibited except with permission of the author.en_US
dc.subjectPhysics, Astronomy and Astrophysics.en_US
dc.titleNeutron star populationsen_US
dc.title.alternativeAspects of neutron star populationsen_US
dc.typetexten_US
dc.typeDissertation-Reproduction (electronic)en_US
thesis.degree.grantorUniversity of Arizonaen_US
thesis.degree.leveldoctoralen_US
dc.identifier.proquest9720706en_US
thesis.degree.disciplineGraduate Collegeen_US
thesis.degree.disciplineAstronomyen_US
thesis.degree.namePh.D.en_US
dc.identifier.bibrecord.b34619793en_US
refterms.dateFOA2018-06-05T19:39:53Z
html.description.abstractThis dissertation clarifies two aspects of neutron-star formation and evolution: the formation of neutron stars through the accretion-induced collapse of white dwarfs and the common envelope evolution of neutron stars. In both cases, we utilize a 1-D lagrangean and 2-D SPH hydrodynamics codes equipped with a broad range of physics including neutrino emission, absorption, and transport, general relativity and dense equations of state. These results are then applied to a Monte-Carlo population synthesis code to study the effects of kicks placed upon neutron stars near the time of their formation. By comparing these results with the current observational data, we find that a bimodal kick distribution of neutron-star kicks is required.


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