Quasinormal modes of Einstein-Gauss-Bonnet-dilaton black holes

Blázquez-Salcedo, Jose Luis; Khoo, Fech Scen; Kunz, Jutta

doi:10.1103/physrevd.96.064008

Cited by 135 publications

(109 citation statements)

References 55 publications

(117 reference statements)

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“…However these attempts are usually limited to spherical symmetry, and they often lead to the conclusion that large classes of black hole solutions are unstable [27,28]. As far as we know, QNM frequencies in modified gravity were computed only in a handful of cases, specifically in Einstein-dilaton-Gauss-Bonnet [29][30][31] and dynamical Chern-Simons [32,33] theories, and even then only for spherically symmetric black hole solutions. These calculations are therefore of limited utility in data analysis applications, both because they must be developed on a case-by-case basis, and because the remnant of a binary black hole merger is almost inevitably a rotating black hole 1 .…”

Section: A the Eikonal Post-kerr Parametrization Schemementioning

confidence: 99%

Post-Kerr black hole spectroscopy

et al. 2017

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One of the central goals of the newborn field of gravitational wave astronomy is to test gravity in the highly nonlinear, strong field regime characterizing the spacetime of black holes. In particular, "black hole spectroscopy" (the observation and identification of black hole quasinormal mode frequencies in the gravitational wave signal) is expected to become one of the main tools for probing the structure and dynamics of Kerr black holes. In this paper we take a significant step towards that goal by constructing a "post-Kerr" quasinormal mode formalism. The formalism incorporates a parametrized but general perturbative deviation from the Kerr metric and exploits the well-established connection between the properties of the spacetime's circular null geodesics and the fundamental quasinormal mode to provide approximate, eikonal limit formulae for the modes' complex frequencies. The resulting algebraic toolkit can be used in waveform templates for ringing black holes with the purpose of measuring deviations from the Kerr metric. As a first illustrative application of our framework, we consider the Johannsen-Psaltis deformed Kerr metric and compute the resulting deviation in the quasinormal mode frequency relative to the known Kerr result.

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Section: A the Eikonal Post-kerr Parametrization Schemementioning

confidence: 99%

Post-Kerr black hole spectroscopy

et al. 2017

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“…Some of these BHs are perturbatively stable [10] and aspects of their phenomenology has been considered in e.g. [11][12][13]. Models where φ = 0 is a consistent truncation are called class II or scalarised-type.…”

Section: Introductionmentioning

confidence: 99%

Spinning black holes in shift-symmetric Horndeski theory

Delgado

Herdeiro

Radu

2020

J. High Energ. Phys.

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We construct spinning black holes (BHs) in shift-symmetric Horndeski theory. This is an Einstein-scalar-Gauss-Bonnet model wherein the (real) scalar field couples linearly to the Gauss-Bonnet curvature squared combination. The BH solutions constructed are stationary, axially symmetric and asymptotically flat. They possess a non-trivial scalar field outside their regular event horizon; thus they have scalar hair. The scalar "charge" is not, however, an independent macroscopic degree of freedom. It is proportional to the Hawking temperature, as in the static limit, wherein the BHs reduce to the spherical solutions found by Sotirou and Zhou. The spinning BHs herein are found by solving non-perturbatively the field equations, numerically. We present an overview of the parameter space of the solutions together with a study of their basic geometric and phenomenological properties. These solutions are compared with the spinning BHs in the Einstein-dilaton-Gauss-Bonnet model and the Kerr BH of vacuum General Relativity. As for the former, and in contrast with the latter, there is a minimal BH size and small violations of the Kerr bound. Phenomenological differences with respect to either the former or the latter, however, are small for illustrative observables, being of the order of a few percent, at most.

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“…to the existence of two black holes of different size, corresponding to the same parameters M and ζ [23]. It has been recently shown in [19] that the additional branch, which in our notations corresponds to the values of p 0.97, is linearly unstable.…”

Section: Black Holes In the Einstein-dilaton-gauss-bonnet Theorymentioning

confidence: 99%

“…An interesting test of our approximate analytical metric could be calculation of gravitational quasinormal modes and comparison of them with those found recently for the numerical metric [19]. Although the quasinormal modes of a four-dimensional dilatonic black holes without Gauss-Bonnet term are well studied by now (see, for example, [25][26][27][28]), the presence of the Gauss-Bonnet term evidently leads to new phenomena and instability for some values of the parameters [19,[29][30][31].…”

Section: Final Remarksmentioning

confidence: 99%

“…Reflection spectrum of accreting black holes was analyzed in [13] and its quasi-period oscillations in [14]. The shadows cast by the black hole were considered in [15,16], while the gravitational quasinormal modes were calculated in [17][18][19]. At the same time, for a number of problems related to simulations of evolution of matter and radiation in the vicinity of a black hole, thermodynamics, Hawking radiation etc., the analytical expression for the metric, even if approximate, would be preferable.…”

Section: Introductionmentioning

confidence: 99%

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Analytical approximation for the Einstein-dilaton-Gauss-Bonnet black hole metric

2017

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We construct an analytical approximation for the numerical black hole metric of P. Kanti, et. al. [Phys. Rev. D 54, 5049 (1996)] in the four-dimensional Einstein-dilaton-Gauss-Bonnet (EdGB) theory. The continued fraction expansion in terms of a compactified radial coordinate, used here, converges slowly when the dilaton coupling approaches its extremal values, but for a black hole far from the extremal state, the analytical formula has a maximal relative error of a fraction of one percent already within the third order of the continued fraction expansion. The suggested analytical representation of the numerical black hole metric is relatively compact and good approximation in the whole space outside the black hole event horizon. Therefore, it can serve in the same way as an exact solution when analyzing particles' motion, perturbations, quasinormal modes, Hawking radiation, accreting disks and many other problems in the vicinity of a black hole. In addition, we construct the approximate analytical expression for the dilaton field.

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Quasinormal modes of Einstein-Gauss-Bonnet-dilaton black holes

Cited by 135 publications

References 55 publications

Post-Kerr black hole spectroscopy

Post-Kerr black hole spectroscopy

Spinning black holes in shift-symmetric Horndeski theory

Analytical approximation for the Einstein-dilaton-Gauss-Bonnet black hole metric

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