Dipolar perturbations of nonbidiagonal black holes in bigravity

TL;DR

This paper analyzes axial dipolar gravitational perturbations of nonbidiagonal black holes in bimetric gravity, revealing superluminal wave propagation in most cases and identifying conditions for physically reasonable solutions.

Contribution

It provides the first analytical solutions for dipolar perturbations on these black holes and clarifies the conditions under which wave propagation remains causal.

Findings

Dipolar gravitational waves are generally superluminal.

Wave velocity increases with distance from the black hole.

Only specific parameter choices yield light-speed propagation.

Abstract

In bimetric gravity, nonbidiagonal solutions describing a static, spherically symmetric, and asymptotically flat black hole are given by a pair of Schwarzschild geometries, one in each metric sector. The two geometries are linked by a nontrivial diffeomorphism, which can be fully determined analytically if the two geometries possess the same isometries. This exact solution depends on four free parameters: the mass parameters of the two black holes, the ratio between the areal radii of the two metrics, and the proportionality constant between their (appropriately normalized) time-translation invariance Killing vector fields. We study the dynamics of axial dipolar perturbations on such a background and obtain general analytical solutions for their evolution. We show that, in general, the characteristic curves followed by dipolar gravitational waves are spacelike with respect to both metrics, and thus the propagation is superluminal. In fact, the velocity of a pulse, as measured by a static observer, turns out to increase with the distance to the black hole. The only exception to this general behavior corresponds to the special case where the two proportionality constants linking the areal radii and the Killing vectors coincide, for which waves travel at the speed of light. Therefore, we conclude that this is the only physically reasonable background, and thus our results restrict the class of viable black-hole solutions in bimetric gravity.