Binary black holes in circular orbits. I. A global spacetime approach

TL;DR

This paper introduces a new spacetime-based method for modeling binary black holes in circular orbits, allowing a rigorous definition of orbital angular velocity and simplifying assumptions to solve Einstein's equations.

Contribution

It presents a global spacetime approach with a conformally flat approximation to analyze binary black holes, differing from previous initial value formulations.

Findings

Defined orbital angular velocity rigorously.

Reduced Einstein equations to five for computational feasibility.

Proposed a method to evaluate errors from conformal flatness approximation.

Abstract

We present a new approach to the problem of binary black holes in the pre-coalescence stage, i.e. when the notion of orbit has still some meaning. Contrary to previous numerical treatments which are based on the initial value formulation of general relativity on a (3-dimensional) spacelike hypersurface, our approach deals with the full (4-dimensional) spacetime. This permits a rigorous definition of the orbital angular velocity. Neglecting the gravitational radiation reaction, we assume that the black holes move on closed circular orbits, which amounts to endowing the spacetime with a helical Killing vector. We discuss the choice of the spacetime manifold, the desired properties of the spacetime metric, as well as the choice of the rotation state for the black holes. As a simplifying assumption, the space 3-metric is approximated by a conformally flat one. The problem is then reduced to solving five of the ten Einstein equations, which are derived here, as well as the boundary conditions on the black hole surfaces and at spatial infinity. We exhibit the remaining five Einstein equations and propose to use them to evaluate the error induced by the conformal flatness approximation. The orbital angular velocity of the system is computed through a requirement which reduces to the classical virial theorem at the Newtonian limit.