Abstract
Abstract Evolution of gravitational perturbations, both in time and frequency domains, is considered for a spherically symmetric black hole in the non-reduced Einstein–Aether theory. It is shown that real oscillation frequency and damping rate are larger for the Einstein–Aether black hole than for the Schwarzschild black hole. This may provide an opportunity to observe aether in the forthcoming experiments with new generation of gravitational antennas.
Highlights
Evolution of gravitational perturbations, both in time and frequency domains, is considered for a spherically symmetric black hole in the non-reduced Einstein-Aether theory
One of the most intriguing issues of modern physics consists in attempts to go beyond local Lorentz symmetry [1]
In theory of gravity, breaking of local Lorentz invariance leads to a general relativity coupled to a dynamical time-like vector field ua, called “aether”
Summary
We used 0, 1, 2, 3 for t, φ, r and θ coordinates respectively. Here we shall consider the axial type of gravitational perturbations. We have the wave-like equation for the radial coordinate d2Ψ dr∗2. Quasi-normal modes of asymptotically AdS black holes have been studies recent years extensively, because of their interpretation in Conformal Field Theory [8] with some specific boundary conditions. One should require natural boundary conditions for QN modes of purely in-going waves at the event horizon and purely out-going waves at spatial infinity. Under these boundary conditions, the quasinormal modes were studied in a great number of papers [9], yet in those cases the background metric and the effective potential were known in analytical form. We shall give only a brief summary of the whole procedure of [5]. Coefficients a(iN), b(iN), a(iB), b(iB) are determined by the fitting procedure.
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