Isolated Horizon structures in quasiequilibrium black hole initial data

Abstract

Isolated horizon conditions enforce the time invariance of both the intrinsic and the extrinsic geometry of a (quasilocal) black hole horizon. Nonexpanding horizons, only requiring the invariance of the intrinsic geometry, have been successfully employed in the (excision) initial data of black holes in instantaneous equilibrium. Here we propose the use of the full isolated horizon structure when solving the elliptic system resulting from the complete set of conformal 3+1 Einstein equations under a quasiequilibrium ansatz prescription. We argue that a set of geometric inner boundary conditions for this extended elliptic system then follows, determining the shape of the excision surface.

4 pages, no figures. Shortened presentation matching the published version

References in corpus (4)

• A constrained scheme for Einstein equations based on Dirac gauge and spherical coordinates
• Mathematical Issues in a Fully-Constrained Formulation of Einstein Equations
• Numerical implementation of isolated horizon boundary conditions
• Excision boundary conditions for the conformal metric

Cited by in corpus (1)

• Excised black hole spacetimes: quasi-local horizon formalism applied to the Kerr example