Energy extremality in the presence of a black hole

TL;DR

This paper derives the first law of black hole mechanics for variations around stationary solutions in Einstein-Maxwell theory, applicable to non-stationary nearby black holes without requiring a bifurcation surface.

Contribution

It provides a 4-dimensional derivation of the first law for arbitrary nearby black holes, extending previous results that depended on bifurcation surfaces.

Findings

First law derived without bifurcation surface assumption.

Applicable to non-stationary black holes close to stationary solutions.

Uses Action variations and Noether operators in the derivation.

Abstract

We derive the so-called first law of black hole mechanics for variations about stationary black hole solutions to the Einstein--Maxwell equations in the absence of sources. That is, we prove that $\delta M=\kappa\delta A+\omega\delta J+VdQ$ where the black hole parameters $M, \kappa, A, \omega, J, V$ and $Q$ denote mass, surface gravity, horizon area, angular velocity of the horizon, angular momentum, electric potential of the horizon and charge respectively. The unvaried fields are those of a stationary, charged, rotating black hole and the variation is to an arbitrary `nearby' black hole which is not necessarily stationary. Our approach is 4-dimensional in spirit and uses techniques involving Action variations and Noether operators. We show that the above formula holds on any asymptotically flat spatial 3-slice which extends from an arbitrary cross-section of the (future) horizon to spatial infinity.(Thus, the existence of a bifurcation surface is irrelevant to our demonstration. On the other hand, the derivation assumes without proof that the horizon possesses at least one of the following two (related)properties: ($i$) it cannot be destroyed by arbitrarily small perturbations of the metric and other fields which may be present, ($ii$) the expansion of the null geodesic generators of the perturbed horizon goes to zero in the distant future.)