Deformed Schwarzschild horizons in second-order perturbation theory: mass, geometry, and teleology

TL;DR

This paper develops second-order perturbation formulas for Schwarzschild black hole horizons, revealing their similarities, localizations, and the non-teleological nature of the event horizon in binary systems.

Contribution

It provides comprehensive second-order perturbation analysis of black hole horizons, clarifying their behavior and differences in binary systems, and challenges previous notions of teleology.

Findings

Event horizon is effectively localized in time.

At linear order, event and apparent horizons coincide.

Hawking masses of horizons remain identical at all orders.

Abstract

In recent years, gravitational-wave astronomy has motivated increasingly accurate perturbative studies of gravitational dynamics in compact binaries. This in turn has enabled more detailed analyses of the dynamical black holes in these systems. For example, Pound et al. [Phys. Rev. Lett. 124, 021101 (2020)] recently computed the surface area of a Schwarzschild black hole's apparent horizon, perturbed by an orbiting body, to second order in the binary's mass ratio. In this paper, we take that as the starting point for a comprehensive study of a perturbed Schwarzschild black hole's apparent and event horizon at second perturbative order, deriving generic formulas for the first- and second-order corrections to the horizons' radial profiles, surface areas, Hawking masses, and intrinsic curvatures. We find that the two horizons are remarkably similar, and that any teleological behavior of the event horizon is suppressed in several ways. Critically, we establish that at all orders, the perturbed event horizon in a small-mass-ratio binary is effectively localized in time. Even more pointedly, the event horizon is identical to the apparent horizon at linear order regardless of the source of perturbation, implying that the seemingly teleological "tidal lead", previously observed in linearly perturbed event horizons, is not genuinely teleological in origin. The two horizons do generically differ at second order, but their Hawking masses remain identical, implying that the event horizon obeys the same energy-flux balance law as the apparent horizon. At least in the case of a binary system, the difference between their surface areas remains extremely small even in the late stages of inspiral. In the course of our analysis, we also numerically illustrate puzzling behaviour in the black hole's motion around the binary's center of mass.