Defining gravitational singularities in general relativity

dc.contributor.authorWurster, James Howarden
dc.contributor.departmentPhysics, Engineering Physics and Astronomyen
dc.contributor.supervisorLake, Kayllen
dc.date2008-07-21 17:13:27.992
dc.date.accessioned2008-07-22T15:19:27Z
dc.date.available2008-07-22T15:19:27Z
dc.date.issued2008-07-22T15:19:27Z
dc.degree.grantorQueen's University at Kingstonen
dc.descriptionThesis (Master, Physics, Engineering Physics and Astronomy) -- Queen's University, 2008-07-21 17:13:27.992en
dc.description.abstractSingularities have been a long-standing problem in general relativity. In all other fields of physics, singularities can be easily located and avoided; in general relativity, singularities have an impact on the creation of the manifold, but, by definition, are not even part of real spacetime. Moreover, all singularities in general relativity cannot be treated in the same manner; thus, the classification of singularities is essential in order to understand them. One important class of singularities is curvature singularities, which, in some cases, can be subclassified as central, shell focusing or shell crossing singularities. We propose to further classify curvature singularities as either gravitational or non-gravitational. In general relativity, a curvature singularity is ``located'' where the scalar invariants of the spacetime are undefined. The gradient field of a non-zero scalar invariant can then be calculated, and the end points of the associated integral curves can be determined. If integral curves are attracted to (i.e. intersect) the singularity, then it is a gravitational singularity; if the integral curves avoid the singularity, then it is a non-gravitational singularity. We will test our method by analysing several different spacetimes, including Friedman-Lemaitre-Robertson-Walker, Schwarzschild, self-similar Vaidya, self-similar Tolman-Bondi, non-self-similar Vaidya, and Kerr spacetimes. We find that in every case studied, the integral curves have specific end points, therefore they can be used to classify a curvature singularity as gravitational or non-gravitational. In Friedman-Lemaitre-Robertson-Walker and Schwarzschild spacetimes, we determined that the a(t) = 0 and r = 0 singularities, respectively, are gravitational singularities. In Vaidya and Tolman-Bondi spacetime, we determine that the massless shell focusing singularities are non-gravitational singularities and that the central singularities (which have mass) are gravitational singularities. We also find that the non-gravitational singularities are the only singularities that have the possibility of being naked. In summary, we can determine which singularities are gravitational and which are non-gravitational by our method of examining the end points of the integral curves, which are constructed from the gradient field of scalar invariants.en
dc.description.degreeM.Sc.en
dc.format.extent4660688 bytes
dc.format.mimetypeapplication/pdf
dc.identifier.urihttp://hdl.handle.net/1974/1332
dc.language.isoengen
dc.relation.ispartofseriesCanadian thesesen
dc.rightsThis publication is made available by the authority of the copyright owner solely for the purpose of private study and research and may not be copied or reproduced except as permitted by the copyright laws without written authority from the copyright owner.en
dc.subjectGeneral relativityen
dc.subjectSingularitiesen
dc.titleDefining gravitational singularities in general relativityen
dc.typethesisen
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