Trapping Horizons as inner boundary conditions for black hole spacetimes

Abstract

We present a set of inner boundary conditions for the numerical construction of dynamical black hole space-times, when employing a 3+1 constrained evolution scheme and an excision technique. These inner boundary conditions are heuristically motivated by the dynamical trapping horizon framework and are enforced in an elliptic subsystem of the full Einstein equation. In the stationary limit they reduce to existing isolated horizon boundary conditions. A characteristic analysis completes the discussion of inner boundary conditions for the radiative modes.

4 pages, no figures, RevTeX4

References in corpus (6)

• Solving Einstein's Equations With Dual Coordinate Frames
• A constrained scheme for Einstein equations based on Dirac gauge and spherical coordinates
• Isolated, slowly evolving, and dynamical trapping horizons: geometry and mechanics from surface deformations
• Area evolution, bulk viscosity and entropy principles for dynamical horizons
• Angular momentum conservation for dynamical black holes
• Numerical implementation of isolated horizon boundary conditions

Cited by in corpus (8)

• New theoretical approaches to black holes
• Mathematical Issues in a Fully-Constrained Formulation of Einstein Equations
• Black holes and black hole thermodynamics without event horizons
• From Geometry to Numerics: interdisciplinary aspects in mathematical and numerical relativity
• Fundamental properties and applications of quasi-local black hole horizons
• Excised black hole spacetimes: quasi-local horizon formalism applied to the Kerr example
• Excision boundary conditions for the conformal metric
• A Black-Hole Excision Scheme for General Relativistic Core-Collapse Supernova Simulations