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Finding black holes in numerical spacetimes

Hughes, Scott A. and Keeton, Charles R., II and Walker, Paul and Walsh, Kevin T. and Shapiro, Stuart L. and Teukolsky, Saul A. (1994) Finding black holes in numerical spacetimes. Physical Review D, 49 (8). pp. 4004-4015. ISSN 2470-0010. https://resolver.caltech.edu/CaltechAUTHORS:20180719-145058836

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Abstract

We have constructed a numerical code that finds black hole event horizons in an axisymmetric rotating spacetime. The spacetime is specified numerically by giving metric coefficients on a spatial grid for a series of time slices. The code solves the geodesic equation for light rays emitted from a suitable sample of points in the evolving spacetime. The algorithm for finding the event horizon employs the apparent horizon, which can form much later than the event horizon, to distinguish between light rays that escape to infinity and light rays that are captured. Simple geometries can be diagnosed on a workstation; more complicated cases are computationally intensive. However, the code is easily parallelized and has been efficiently run on the IBM SP-1 parallel machine. We have illustrated the use of the event horizon code on two cases. One is the head-on collision of two black holes that form from the collapse of collisionless matter, coalescing to a single Schwarzschild black hole. The other is the collapse of a rotating toroid to form a Kerr black hole. In this case the horizon initially appears with a toroidal topology. This is the first known example of this phenomenon.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1103/PhysRevD.49.4004DOIArticle
ORCID:
AuthorORCID
Teukolsky, Saul A.0000-0001-9765-4526
Additional Information:© 1994 American Physical Society. (Received 5 November 1993) We thank Michael Blanton and Michael Chia for assistance with visualization and for help developing the horizon finder algorithm. We also thank Andrew Abrahams for useful discussions and Michael Piper for programming assistance in the early stages of the project. S.H., C.K, P.W., and K.W. were supported in part by the Research Experiences for Undergraduates program of the National Science Foundation. This research was supported in part by NSF Grants Nos. AST 91-19475 and PHY 90-07834 and NASA grant NAGW-2364 at Cornell University. Computations were performed at the Cornell Center for Theory and Simulation in Science and Engineering, which is supported in part by the National Science Foundation, IBM Corporation, New York State, and the Cornell Research Institute.
Funders:
Funding AgencyGrant Number
NSFAST 91-19475
NSFPHY 90-07834
NASANAGW-2364
IBM Corp.UNSPECIFIED
State of New YorkUNSPECIFIED
Cornell Research InstituteUNSPECIFIED
Issue or Number:8
Classification Code:PACS number(s): 04.25.Dm, 97.60.Lf
Record Number:CaltechAUTHORS:20180719-145058836
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20180719-145058836
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:88020
Collection:CaltechAUTHORS
Deposited By: George Porter
Deposited On:19 Jul 2018 22:11
Last Modified:22 Nov 2019 09:58

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