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Finding apparent horizons in dynamic 3D numerical spacetimes

Peter Anninos1, Karen Camarda1,4,6, Joseph Libson1,4, Joan Massó1,2,6, Edward Seidel1,4,6,7, and Wai-Mo Suen3,5

  • 1National Center for Supercomputing Applications, 605 E. Springfield Avenue, Champaign, Illinois 61820
  • 2Departament de Física, Universitat de les Illes Balears, E-07071 Palma de Mallorca, Spain
  • 3McDonnell Center for the Space Sciences, Department of Physics, Washington University, St. Louis, Missouri 63130
  • 4Department of Physics, University of Illinois at Urbana-Champaign, Illinois 61801
  • 5Physics Department, Chinese University of Hong Kong, Shatin, Hong Kong
  • 6Max-Planck-Institut für Gravitationsphysik, Schlaatzweg 1, 14473 Potsdam, Germany
  • 7Department of Astronomy, University of Illinois, Urbana, Illinois 61801

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Phys. Rev. D 58, 024003 – Published 8 June, 1998

DOI: https://doi.org/10.1103/PhysRevD.58.024003

Abstract

We have developed a general method for finding apparent horizons in 3D numerical relativity. Instead of solving for the partial differential equation describing the location of the apparent horizons, we expand the closed 2D surfaces in terms of symmetric trace-free tensors and solve for the expansion coefficients using a minimization procedure. Our method is applied to a number of different spacetimes, including numerically constructed spacetimes containing highly distorted axisymmetric black holes in spherical coordinates, and 3D rotating, and colliding black holes in Cartesian coordinates.

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Phys. Rev. D 58, 024003– Published 8 June, 1998
  • Received 29 August 1996

© 1998 American Physical Society

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