General theories of linear gravitational perturbations to a Schwarzschild black hole

Tattersall, Oliver J.; Ferreira, Pedro G.; Lagos, Macarena

doi:10.1103/physrevd.97.044021

Cited by 55 publications

(73 citation statements)

References 75 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…orbiting stars around BHs [5][6][7], or BH imaging [8][9][10]), QNM carry information on the dynamical regime of gravity and thus provide crucial new information. In particular, in the case of a massive scalar field conformally coupled to gravity, the BH stationary solution is a Kerr metric, as in GR, while the QNM spectrum will generically be given by a linear superposition of the normal GR spectrum and the scalar field spectrum [11]. Studying this scalar field spectrum then will help understand one of the possible deviations from GR that can be tested in the future with a detection of QNM.…”

Section: Introductionmentioning

confidence: 99%

Anomalous decay rate of quasinormal modes

2020

Self Cite

View full text Add to dashboard Cite

The decay timescales of the quasinormal modes of a massive scalar field have an intriguing behaviour: they either grow or decay with increasing angular harmonic numbers , depending on whether the mass of the scalar field is small or large. We identify the properties of the effective potential of the scalar field that leads to this behaviour and characterize it in detail. If the scalar field is non-minimally coupled, considered here, the scalar quasinormal modes will leak into the gravitational wave signal and will have decaying times that are comparable or smaller than those typical in General Relativity. Hence, these modes could be detectable in the future. Finally, we find that the anomalous behaviour in the decay timescales of quasinormal modes is present in a much larger class of models beyond a simple massive scalar field. * mlagos@kicp.uchicago.edu † pedro.ferreira@physics.ox.ac.uk ‡ oliver.tattersall@physics.ox.ac.uk 1 From the publicly available data in [16], one can check that, for any given azimuthal number m, the QNM are such that |ω I | grows with for all values of the BH's dimensionless spin a = J/M 2 .

show abstract

Section: Introductionmentioning

confidence: 99%

Anomalous decay rate of quasinormal modes

2020

Self Cite

View full text Add to dashboard Cite

show abstract

“…The resulting eikonal expressions, although somewhat unwieldy and markedly more complicated than those of Paper I, should encompass a large class of black holes beyond GR. The algebraic complexity of our results is the main reason we have not attempted a similar analysis (although such analysis should be feasible) for the coupled system of three black hole perturbation equations that appear in generalised vector-tensor [19] and in Einstein-Maxwell-dilaton theories [29]. As was the case for the perturbation equations of Paper I, we have been able to show that the eikonal QNM can be associated with the peak of an effective potential although no correspondence to a geodesic photon ring appears to exist (this issue was explored in detail in [32]).…”

Section: Discussionmentioning

confidence: 99%

“…We consider perturbed non-GR black holes described by a general system of wave equations with two coupled scalar-tensor field degrees of freedom {Θ, ψ}. Our equations are supposed to be theory-agnostic but they do include, for instance, the perturbation equations of Schwarzschild black holes within the framework of the generalised class of scalar-tensor theories discussed in [19]. Although we assume spherically symmetric black holes, we can also allow for the possibility of first-order rotational corrections.…”

Section: The Coupled Wave Equationsmentioning

confidence: 99%

“…A violation of this hypothesis would hint towards new physics beyond GR [17]. This has motivated considerable effort in modeling the QNM spectrum of black holes outside the Kerr paradigm, ranging from model-independent parametrisations [18][19][20][21][22][23] to calculations done in specific beyond-GR theories, e.g. [24][25][26][27][28][29][30][31].…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Eikonal quasinormal modes of black holes beyond general relativity. II. Generalized scalar-tensor perturbations

Silva

Glampedakis

2020

Phys. Rev. D

View full text Add to dashboard Cite

Black hole 'spectroscopy', i.e. the identification of quasinormal mode frequencies via gravitational wave observations, is a powerful technique for testing the general relativistic nature of black holes. In theories of gravity beyond general relativity perturbed black holes are typically described by a set of coupled wave equations for the tensorial field and the extra scalar/vector degrees of freedom, thus leading to a theory-specific quasinormal mode spectrum. In this paper we use the eikonal/geometric optics approximation to obtain analytic formulae for the frequency and damping rate of the fundamental quasinormal mode of a generalised, theory-agnostic system of equations describing coupled scalar-tensor perturbations of spherically symmetric black holes. Representing an extension of our recent work, the present model includes a massive scalar field, couplings through the field derivatives and first-order frame-dragging rotational corrections. Moving away from spherical symmetry, we consider the simple model of the scalar wave equation in a general stationary-axisymmetric spacetime and use the eikonal approximation to compute the quasinormal modes associated with equatorial and nonequatorial photon rings. * hosilva@illinois.edu † kostas@um.es

show abstract

“…We will assume that the UV cutoff of the dark energy EFT, and 3 Note that the frequencies of the LIGO measurement of GW170817 are close to Λ 3 , so additional assumptions about the UV physics are implicitly made when using this measurement to constrain such 'cosmological' operators suppressed by Λ 3 [19]. 4 The exact definition of the operators is given below in Eq. (6), here we are just keeping track schematically of the number of fields and derivatives.…”

Section: Introduction and Setupmentioning

confidence: 99%

Black hole ringdown as a probe for dark energy

2020

View full text Add to dashboard Cite

Under the assumption that a dynamical scalar field is responsible for the current acceleration of the Universe, we explore the possibility of probing its physics in black hole merger processes with gravitational wave interferometers. Remaining agnostic about the microscopic physics, we use an effective field theory approach to describe the scalar dynamics. We investigate the case in which some of the higher derivative operators, that are highly suppressed on cosmological scales, instead become important on typical distances for black holes. If a coupling to the Gauss-Bonnet operator is one of them, a non-trivial background profile for the scalar field can be sourced in the surrounding of the black hole, resulting in a potentially large amount of 'hair'. In turn, this can induce sizeable modifications to the spacetime geometry or a mixing between the scalar and the gravitational perturbations. Both effects will ultimately translate into a modification of the quasi-normal mode spectrum in a way that is also sensitive to other operators besides the one sourcing the scalar background. The presence of deviations from the predictions of general relativity in the observed spectrum can therefore serve as a window onto dark energy physics.

show abstract

General theories of linear gravitational perturbations to a Schwarzschild black hole

Cited by 55 publications

References 75 publications

Anomalous decay rate of quasinormal modes

Anomalous decay rate of quasinormal modes

Eikonal quasinormal modes of black holes beyond general relativity. II. Generalized scalar-tensor perturbations

Black hole ringdown as a probe for dark energy

Contact Info

Product

Resources

About