Radiation tails and boundary conditions for black hole evolutions
General Relativity and Quantum Cosmology
2009-11-10 v1
Abstract
In numerical computations of Einstein's equations for black hole spacetimes, it will be necessary to use approximate boundary conditions at a finite distance from the holes. We point out here that ``tails,'' the inverse power-law decrease of late-time fields, cannot be expected for such computations. We present computational demonstrations and discussions of features of late-time behavior in an evolution with a boundary condition.
Cite
@article{arxiv.gr-qc/0401092,
title = {Radiation tails and boundary conditions for black hole evolutions},
author = {Elspeth W. Allen and Elizabeth Buckmiller and Lior M. Burko and Richard H. Price},
journal= {arXiv preprint arXiv:gr-qc/0401092},
year = {2009}
}
Comments
submitted to Phys. Rev. D