Dragging of inertial frames in the composed black-hole–ring system

Shahar Hod

doi:10.1140/epjc/s10052-015-3787-9

Abstract

A well-established phenomenon in general relativity is the dragging of inertial frames by a spinning object. In particular, due to the dragging of inertial frames by a ring orbiting a central black hole, the angular-velocity of the black-hole horizon in the composed black-hole-ring system is no longer related to the black-hole angular-momentum by the simple Kerr-like (vacuum) relation $\Omega^{\text{Kerr}}_{\text{H}}(J_{\text{H}})=J_{\text{H}}/2M^2R_{\text{H}}$. Will has performed a perturbative treatment of the composed black-hole-ring system in the regime of slowly rotating black holes and found the explicit relation $\Omega^{\text{BH-ring}}_{\text{H}}(J_{\text{H}}=0,J_{\text{R}},R)=2J_{\text{R}}/R^3$ for the angular-velocity of a central black hole with zero angular-momentum. Analyzing a sequence of black-hole-ring configurations with adiabatically varying (decreasing) circumferential radii, we show that the expression found by Will implies a smooth transition of the central black-hole angular-velocity from its asymptotic near-horizon value $\Omega^{\text{BH-ring}}_{\text{H}}(J_{\text{H}}=0,J_{\text{R}},R\to R^{+}_{\text{H}})$ to its final Kerr (vacuum) value $\Omega^{\text{Kerr}}_{\text{H}}(J^{\text{new}}_{\text{H}})$. We use this important observation in order to generalize the result of Will to the regime of black-hole-ring configurations in which the central black holes possess non-zero angular momenta. Remarkably, we find the simple universal relation $\Delta\Omega_{\text{H}}\equiv\Omega^{\text{BH-ring}}_{\text{H}}(J_{\text{H}},J_{\text{R}},R\to R^{+}_{\text{H}})-\Omega^{\text{Kerr}}_{\text{H}}(J_{\text{H}})={{J_{\text{R}}}/{4M^3}}$ for the asymptotic deviation of the black-hole angular-velocity in the composed black-hole-ring system from the corresponding angular-velocity of the unperturbed (vacuum) Kerr black hole with the same angular-momentum.

Highlights

The gravitational two-body problem has attracted much attention over the years from both physicists and mathematicians
Of the black-hole horizon in the composed black-hole–ring system is no longer related to the black-hole angular momentum
It is highly important to explore the physics of a central black hole surrounded by an orbiting ring: it is expected that this composed two-body system may be formed as an intermediate stage in the gravitational collapse of a compact spinning star to form a black hole [1,2,3]

Summary

Introduction

The gravitational two-body problem has attracted much attention over the years from both physicists and mathematicians. It is highly important to explore the physics of a central black hole surrounded by an orbiting ring: it is expected that this composed two-body system may be formed as an intermediate stage in the gravitational collapse of a compact spinning star to form a black hole [1,2,3]. The coalescence of two compact objects may produce a composed black-hole–ring system [1,2,3] In addition to these astrophysical motivations, it is highly interesting to explore the composed black-hole–ring system in order to understand how an exterior matter configuration affects the physical properties of central black holes [1,2,3,4,5]. It was shown in [4] that, due to the well-known phenomenon of dragging of inertial frames by the orbiting ring, the angular velocity

Objectives

Conclusion