An approximate binary-black-hole metric
General Relativity and Quantum Cosmology
2009-10-31 v2
Abstract
An approximate solution to Einstein's equations representing two widely-separated non-rotating black holes in a circular orbit is constructed by matching a post-Newtonian metric to two perturbed Schwarzschild metrics. The spacetime metric is presented in a single coordinate system valid up to the apparent horizons of the black holes. This metric could be useful in numerical simulations of binary black holes. Initial data extracted from this metric have the advantages of being linked to the early inspiral phase of the binary system, and of not containing spurious gravitational waves.
Cite
@article{arxiv.gr-qc/9912113,
title = {An approximate binary-black-hole metric},
author = {Kashif Alvi},
journal= {arXiv preprint arXiv:gr-qc/9912113},
year = {2009}
}
Comments
20 pages, 1 figure; some changes in Sec. IV B,C and Sec. V