Mandel, Ilya (2005) Geometry of a naked singularity created by standing waves near a Schwarzschild horizon, and its application to the binary black hole problem. Physical Review D, 72 (8). Art. No. 084025. ISSN 05562821. http://resolver.caltech.edu/CaltechAUTHORS:MANprd05

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Abstract
The most promising way to compute the gravitational waves emitted by binary black holes (BBHs) in their last dozen orbits, where postNewtonian techniques fail, is a quasistationary approximation introduced by Detweiler and being pursued by Price and others. In this approximation the outgoing gravitational waves at infinity and downgoing gravitational waves at the holes’ horizons are replaced by standing waves so as to guarantee that the spacetime has a helical Killing vector field. Because the horizon generators will not, in general, be tidally locked to the holes’ orbital motion, the standing waves will destroy the horizons, converting the black holes into naked singularities that resemble black holes down to near the horizon radius. This paper uses a spherically symmetric, scalarfield model problem to explore in detail the following BBH issues: (i) The destruction of a horizon by the standing waves. (ii) The accuracy with which the resulting naked singularity resembles a black hole. (iii) The conversion of the standingwave spacetime (with a destroyed horizon) into a spacetime with downgoing waves by the addition of a "radiationreaction field." (iv) The accuracy with which the resulting downgoing waves agree with the downgoing waves of a true blackhole spacetime (with horizon). The model problem used to study these issues consists of a Schwarzschild black hole endowed with spherical standing waves of a scalar field, whose wave frequency and nearhorizon energy density are chosen to match those of the standing gravitational waves of the BBH quasistationary approximation. It is found that the spacetime metric of the singular, standingwave spacetime, and its radiationreactionfieldconstructed downgoing waves are quite close to those for a Schwarzschild black hole with downgoing waves—sufficiently close to make the BBH quasistationary approximation look promising for nontidallylocked black holes.
Item Type:  Article 

Additional Information:  © 2005 The American Physical Society. Received 30 May 2005; published 25 October 2005. I am very grateful to my advisor, Kip S. Thorne, for posing this research project and for his extremely patient guidance. Jonathan Gair, Lee Lindblom, Robert Owen, Frans Pretorius and Mark A. Scheel of the TAPIR group at Caltech made many helpful suggestions, as did Ronald J. Adler and Alexander S. Silbergleit of the GPB theory seminar at Stanford, and Richard Price of UT Brownsville. I was partially supported by NSF Grant No. PHY0099568 and NASA Grant No. NAG512834. 
Subject Keywords:  black holes; gravitational waves; Schwarzschild metric; spacetime configurations 
Record Number:  CaltechAUTHORS:MANprd05 
Persistent URL:  http://resolver.caltech.edu/CaltechAUTHORS:MANprd05 
Alternative URL:  http://dx.doi.org/10.1103/PhysRevD.72.084025 
Usage Policy:  No commercial reproduction, distribution, display or performance rights in this work are provided. 
ID Code:  3418 
Collection:  CaltechAUTHORS 
Deposited By:  Lindsay Cleary 
Deposited On:  06 Jun 2006 
Last Modified:  26 Dec 2012 08:54 
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