Infinite Red-Shifts in General Relativity

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dc.contributor.authorMisner, Charles W
dc.contributor.authorBeckedorff, David L
dc.date.accessioned2007-02-07T17:02:44Z
dc.date.available2007-02-07T17:02:44Z
dc.date.issued1967
dc.descriptionThis Cornell 1967 publication is a taped transcript of a talk given in June 1963. It presented a soon-to-be-standard insight into idealized spherical gravitational collapse, and may have influenced significant participants at that meeting such as Wheeler, Penrose, and Sciama. For comments on the impact of this work see: K. S. Thorne "Black Holes ..." (Norton 1994) p.246; J. A. Wheeler and K. Ford "Geons, Black Holes, ..." (Norton 1998) p.295; M. Bartusiak "Einstein's Unfinished Sumphony" (Joseph Henry Press 2000) p.61en
dc.description.abstractThe Oppenheimer-Snyder description of continued gravitational collapse is reformulated as a matching together of two familiar solutions of the Einstein gravitational equations. From one solution, the Friedmann cosmology with zero-pressure matter, one selects the interior of a sphere whose points move on timelike geodesics. From the other solution one selects the exterior of such a sphere in the vacuum Schwarzschild solution. For the expected choice of parameters (sphere circumference, interior density, exterior mass) these can be fit together smoothly enough to satisfy the Einstein equations. The matching conditions are that the first and second fundamental forms at the joining 3-surface agree. The description of this collapsing ball of matter survives its passage through Finkelstein's (1958) smooth unidirectional membrane€ at r=2M and is most conveniently presented using the Kruskal coordinates for the Schwarzschild solution. This project was proposed and designed by Misner (choice of solutions and matching requirements), but the execution and first written presentation were carried out by Beckedorff and provided his Princeton senior thesis in April 1962. ( http://www.physics.umd.edu/grt/cwm/Beckedorff1962.pdf ) In this 1963 presentation Misner emphasizes that the properties of matter at high densities are irrelevant to the question of whether such a collapse can occur for sufficiently massive objects. The detailed computations by Beckedorff are here linked in an appended file.en
dc.description.sponsorshipReprinted from The Nature of Time, edited by T. Gold. Copyright © 1967 by Cornell University. Used by permission of Cornell University Press.en
dc.format.extent45774 bytes
dc.format.extent641009 bytes
dc.format.mimetypetext/html
dc.format.mimetypeapplication/pdf
dc.identifier.citationT. Gold, "The Nature of Time", Chapter 6en
dc.identifier.otherQB209.G56
dc.identifier.otherORCID ID: http://orcid.org/0000-0003-4888-5744en
dc.identifier.urihttp://hdl.handle.net/1903/4280
dc.language.isoen_USen
dc.publisherCornell University Pressen
dc.relation.isAvailableAtCollege of Computer, Mathematical & Physical Sciencesen_us
dc.relation.isAvailableAtPhysicsen_us
dc.relation.isAvailableAtDigital Repository at the University of Marylanden_us
dc.relation.isAvailableAtUniversity of Maryland (College Park, Md.)en_us
dc.subjectcontinued gravitational contractionen
dc.subjectOppenheimer-Snyderen
dc.subjectgravitational collapseen
dc.subjectblack holesen
dc.subjectSchwarzschild metricen
dc.subjectFriedmann cosmologyen
dc.subjectFinkenstein coordinatesen
dc.subjectKruskal coordinatesen
dc.subjectgeneral relativityen
dc.subjectEinstein equationsen
dc.titleInfinite Red-Shifts in General Relativityen
dc.typeBook chapteren

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