Event horizons in numerical relativity: Methods and tests

Joseph Libson, Joan Massó, Edward Seidel, Wai-Mo Suen, and Paul Walker
Phys. Rev. D 53, 4335 – Published 15 April 1996
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Abstract

This is the first paper in a series on event horizons in numerical relativity. In this paper we present methods for obtaining the location of an event horizon in a numerically generated spacetime. The location of an event horizon is determined based on two key ideas: (1) integrating backward in time and (2) integrating the whole horizon surface. The accuracy, efficiency and robustness of the methods are examined with various sample spacetimes, including both analytic (Schwarzschild and Kerr) and numerically generated black holes. The numerically evolved spacetimes contain highly distorted black holes, rotating black holes, and colliding black holes. In all cases studied, our methods can find event horizons to within a very small fraction of a grid zone. © 1996 The American Physical Society.

  • Received 11 September 1995

DOI:https://doi.org/10.1103/PhysRevD.53.4335

©1996 American Physical Society

Authors & Affiliations

Joseph Libson, Joan Massó, Edward Seidel, Wai-Mo Suen, and Paul Walker

  • National Center for Supercomputing Applications, Beckman Institute, 405 N. Mathews Avenue, Urbana, Illinois 61801
  • Departament de Física, Universitat de les Illes Balears, E-07071 Palma de Mallorca, Spain
  • Department of Physics, University of Illinois, Urbana, Illinois 61801
  • McDonnell Center for the Space Sciences, Department of Physics, Washington University, St. Louis, Missouri 63130

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Issue

Vol. 53, Iss. 8 — 15 April 1996

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