Perturbative, Post-Newtonian, and General Relativistic Dynamics of Black Hole Binaries

TL;DR

This paper reviews recent comparisons of different approximation and numerical methods in modeling black hole binary dynamics, showing they agree well within their valid regimes.

Contribution

It provides a comparative analysis of post-Newtonian, perturbation, numerical relativity, and effective-one-body approaches for black hole binaries.

Findings

All methods agree very well within their common domain of validity.

The comparisons validate the consistency of different approximation schemes.

The study enhances confidence in modeling black hole binary dynamics.

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.