Gravitational perturbations of a Kerr black hole in<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mi>f</mml:mi><mml:mo mathvariant="bold" stretchy="false">(</mml:mo><mml:mi>R</mml:mi><mml:mo mathvariant="bold" stretchy="false">)</mml:mo></mml:math>gravity

Suvorov, Arthur G.

doi:10.1103/physrevd.99.124026

Cited by 30 publications

(29 citation statements)

References 81 publications

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“…In the present work we consider a stealth rotating black hole solution obtained very recently [23] in the context of Degenerate Higher Order Scalar Tensor (DHOST) theories [24][25][26], 1 See [19] for Einstein-Maxwell theory, [20] for recent results in f (R) theory and [21,22] for slowly rotating black holes without hair in Horndeski theories which represent the most general class of covariant scalartensor theories with a single scalar degree of freedom (see [27] for a review). This black hole solution is characterised by an exact Kerr (or, more generally, Kerr-de Sitter) geometry and a non-trivial scalar field which can be identified with families of geodesics of the spacetime itself 2 .…”

Section: Introductionmentioning

confidence: 99%

Perturbations of a rotating black hole in DHOST theories

Charmousis

Crisostomi

Langlois

et al. 2019

Class. Quantum Grav.

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We study linear perturbations of a rotating black hole solution that has been recently discovered in degenerate higher-order scalar-tensor (DHOST) theories. We find a parametrization which permits the explicit resolution of the scalar perturbation while the tensor perturbation is obtained as a Teukolsky equation supplemented by an effective source term. The effective source term is related to the black hole hair and can be computed exactly for any value of the black hole spin. We discuss how the perturbations of the geometry and thus the emitted gravitational waves could be modified in comparison with general relativity.

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Section: Introductionmentioning

confidence: 99%

Perturbations of a rotating black hole in DHOST theories

Charmousis

Crisostomi

Langlois

et al. 2019

Class. Quantum Grav.

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“…2, but is also dynamical; Ricci modes can exist even in the f (R) subcase (e.g. [19]). A thorough check of these conditions involves detailed calculations on a case-by-case basis that will be conducted elsewhere.…”

Section: A Mixed Scalar-f(r) Gravitymentioning

confidence: 99%

A family of solutions to the inverse problem in gravitation: building a theory around a metric

Suvorov

2021

Gen Relativ Gravit

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A method is presented to construct a particular, non-minimally coupled scalar–tensor theory such that a given metric is an exact vacuum solution in that theory. In contrast to the standard approach in studies of gravitational dynamics, where one begins with an action and then solves the equations of motion, this approach allows for an explicit theory to be built around some pre-specified geometry. Starting from a parameterized black hole spacetime with generic, non-Kerr hairs, it is shown how an overarching family of theories can be designed to fit the metric exactly.

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“…See also Ref. [64] where it was detailed how one can test beyond-GR theories of gravity, even for Kerr BHs [65] if one considers their perturbations.…”

Section: Introductionmentioning

confidence: 99%

Probing beyond-Kerr spacetimes with inspiral-ringdown corrections to gravitational waves

Carson

Yagi

2020

Phys. Rev. D

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Gravitational waves from the explosive merger of distant black holes are encoded with details regarding the complex extreme-gravity spacetime present at their source. Famously described by the Kerr spacetime metric for rotating black holes in general relativity, what if effects beyond this theory are present? One way to efficiently test this hypothesis is to first obtain a metric which parametrically deviates from the Kerr metric in a model-independent way. Given such a metric, one can then predict the ensuing corrections to both the inspiral and ringdown portions of the gravitational waveform for black holes present in the new spacetime. With these tools in hand, one can then test gravitational wave signals for such effects by two different methods, (i) inspiralmerger-ringdown consistency test, and (ii) parameterized test. In this paper, we demonstrate the exact recipe one needs to do just this. We first derive parameterized corrections to the waveform inspiral, ringdown, and remnant properties for a generic non-Kerr spacetime and apply this to two example beyond-Kerr spacetimes each parameterized by a single non-Kerr parameter. We then predict the beyond-Kerr parameter magnitudes required in an observed gravitational wave signal to be statistically inconsistent with the Kerr case in general relativity. We find that the two methods give very similar bounds. The constraints found with existing gravitational-wave events are comparable to those from x-ray observations, while future gravitational-wave observations using Cosmic Explorer (Laser Interferometer Space Antenna) can improve such bounds by two (three) orders of magnitude.

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Gravitational perturbations of a Kerr black hole inf(R)gravity

Cited by 30 publications

References 81 publications

Perturbations of a rotating black hole in DHOST theories

Perturbations of a rotating black hole in DHOST theories

A family of solutions to the inverse problem in gravitation: building a theory around a metric

Probing beyond-Kerr spacetimes with inspiral-ringdown corrections to gravitational waves

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