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Phys. Rev. D 67, 024018 (2003) [14 pages]

Introduction to isolated horizons in numerical relativity

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Olaf Dreyer*
Perimeter Institute for Theoretical Physics, 35 King Street North, Waterloo, Ontario, Canada N2J 2W9

Badri Krishnan† and Deirdre Shoemaker‡
Center for Gravitational Physics and Geometry and Center for Gravitational Wave Physics, Department of Physics, Penn State University, University Park, Pennsylvania 16802

Erik Schnetter§
Theoretische Astrophysik, Universität Tübingen, Auf der Morgenstelle, 72076 Tübingen, Germany

Received 10 June 2002; published 17 January 2003

We present a coordinate-independent method for extracting the mass (MΔ) and angular momentum (JΔ) of a black hole in numerical simulations. This method, based on the isolated horizon framework, is applicable both at late times when the black hole has reached equilibrium, and at early times when the black holes are widely separated. Assuming that the spatial hypersurfaces used in a given numerical simulation are such that apparent horizons exist and have been located on these hypersurfaces, we show how JΔ and MΔ can be determined in terms of only those quantities which are intrinsic to the apparent horizon. We also present a numerical method for finding the rotational symmetry vector field (required to calculate JΔ) on the horizon.

© 2003 The American Physical Society

URL:
http://link.aps.org/doi/10.1103/PhysRevD.67.024018
DOI:
10.1103/PhysRevD.67.024018
PACS:
04.25.Dm, 04.70.Bw

*Electronic address: odreyer@perimeterinstitute.ca

†Present address: Max Planck Institut für Gravitationsphysik, Am Mühlenberg 1, D-14476 Golm, Germany. Electronic address: badkri@aei-potsdam.mpg.de

‡Present address: Center for Radiophysics and Space Research, Cornell University, Ithaca, NY 14853. Electronic address: deirdre@astro.cornell.edu

§Electronic address: schnetter@uni-tuebingen.de

 
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