A Hamiltonian Approach to the Mass of Isolated Black Holes
arXiv:gr-qc/9908006 · doi:10.1063/1.1301582
Abstract
Boundary conditions defining a non-rotating isolated horizon are given in Einstein-Maxwell theory. A spacetime representing a black hole which itself is in equilibrium but whose exterior contains radiation admits such a horizon. Inspired by Hamiltonian mechanics, a (quasi-)local definition of isolated horizon mass is formulated. Although its definition does not refer to infinity, this mass takes the standard value in a Reissner-Nordstrom solution. Furthermore, under certain technical assumptions, the mass of an isolated horizon is shown to equal the future limit of the Bondi energy.
5 pages, LaTeX 2.09, 1 eps figure. To appear in the proceedings of the Eighth Canadian Conference on General Relativity and Relativistic Astrophysics