Black-hole horizons as probes of black-hole dynamics I: post-merger recoil in head-on collisions

TL;DR

This paper investigates black-hole horizon geometry during binary black hole mergers, using numerical relativity to analyze recoil velocities and horizon dynamics, providing new tools to understand strong-field gravitational phenomena.

Contribution

It introduces a novel correlation between horizon geometry and gravitational wave fluxes to analyze recoil in black-hole mergers, extending previous methods with a geometric approach.

Findings

Successfully tracked recoil dynamics through horizon geometry

Validated the effective-curvature vector as a probe of spacetime dynamics

Connected local horizon properties with asymptotic gravitational wave fluxes

Abstract

The understanding of strong-field dynamics near black-hole horizons is a long-standing and challenging prob- lem in general relativity. Recent advances in numerical relativity and in the geometric characterization of black- hole horizons open new avenues into the problem. In this first paper in a series of two, we focus on the analysis of the recoil occurring in the merger of binary black holes, extending the analysis initiated in [1] with Robinson- Trautman spacetimes. More specifically, we probe spacetime dynamics through the correlation of quantities defined at the black-hole horizon and at null infinity. The geometry of these hypersurfaces responds to bulk gravitational fields acting as test screens in a scattering perspective of spacetime dynamics. Within a 3 + 1 approach we build an effective-curvature vector from the intrinsic geometry of dynamical-horizon sections and correlate its evolution with the flux of Bondi linear momentum at large distances. We employ this setup to study numerically the head-on collision of nonspinning black holes and demonstrate its validity to track the qualita- tive aspects of recoil dynamics at infinity. We also make contact with the suggestion that the antikick can be described in terms of a "slowness parameter" and how this can be computed from the local properties of the horizon. In a companion paper [2] we will further elaborate on the geometric aspects of this approach and on its relation with other approaches to characterize dynamical properties of black-hole horizons.