Self-force as a cosmic censor in the Kerr overspinning problem

TL;DR

This paper demonstrates that when self-force effects are properly included, overspinning a Kerr black hole beyond its extremal limit is prevented, supporting the cosmic censorship conjecture.

Contribution

It provides a numerical calculation of self-force effects showing they prevent overspinning in the Kerr black hole scenario within first-order approximation.

Findings

Self-force effects prevent overspinning in most cases.

Possibility of reaching extremality exists at first-order self-force approximation.

Higher-order effects are needed to conclusively rule out overspinning.

Abstract

It is known that a near-extremal Kerr black hole can be spun up beyond its extremal limit by capturing a test particle. Here we show that overspinning is always averted once back-reaction from the particle's own gravity is properly taken into account. We focus on nonspinning, uncharged, massive particles thrown in along the equatorial plane, and work in the first-order self-force approximation (i.e., we include all relevant corrections to the particle's acceleration through linear order in the ratio, assumed small, between the particle's energy and the black hole's mass). Our calculation is a numerical implementation of a recent analysis by two of us [Phys.\ Rev.\ D {\bf 91}, 104024 (2015)], in which a necessary and sufficient "censorship" condition was formulated for the capture scenario, involving certain self-force quantities calculated on the one-parameter family of unstable circular geodesics in the extremal limit. The self-force information accounts both for radiative losses and for the finite-mass correction to the critical value of the impact parameter. Here we obtain the required self-force data, and present strong evidence to suggest that captured particles never drive the black hole beyond its extremal limit. We show, however, that, within our first-order self-force approximation, it is possible to reach the extremal limit with a suitable choice of initial orbital parameters. To rule out such a possibility would require (currently unavailable) information about higher-order self-force corrections.