Authors: Alexandre Le Tiec
Date: 30 Sep 2011
Abstract: The orbital motion of inspiralling and coalescing black hole binaries can be investigated using a variety of approximation schemes and numerical methods within general relativity: post-Newtonian expansions, black hole perturbation theory, numerical relativity, and the effective-one-body formalism. We review two recent comparisons of the predictions from these various techniques. Both comparisons rely on the calculation of a coordinate invariant relation, in the case of non-spinning binary black holes on quasi-circular orbits. All methods are shown to agree very well in their common domain of validity.
© M. Vallisneri 2012 — last modified on 2010/01/29
Tantum in modicis, quantum in maximis