Quasinormal modes of black holes in Horndeski gravity

Tattersall, Oliver J.; Ferreira, Pedro G.

doi:10.1103/physrevd.97.104047

Cited by 93 publications

(111 citation statements)

References 60 publications

(113 reference statements)

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“…(37) can also be derived by calculating the QNMs using the analytic series expansion method of [40] and looking at the sub-leading term for ω I in the eikonal limit. Analytic expressions for the QNMs of massive scalar fields obtained through the series expansion method of [40] can be found in [15]. For a massive scalar field we have that…”

Section: Other Potentialsmentioning

confidence: 99%

Anomalous decay rate of quasinormal modes

2020

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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 .

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Section: Other Potentialsmentioning

confidence: 99%

Anomalous decay rate of quasinormal modes

2020

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“…These departures can be due to extra charges, a modified theory of gravity, environmental effects, etcetera, and we wish to develop a generic framework that can accommodate various special cases. GR corrections might affect the ringdown in two ways: by predicting a spinning BH other than Kerr [11,12,15,50,51,53,57,66], or (even if GR BHs are still solutions of the theory) by affecting the dynamics of the perturbations [40,[67][68][69][70][71]. In both cases, the ringdown modes will acquire corrections proportional to the fundamental coupling constant(s) of the theory.…”

Section: Introductionmentioning

confidence: 99%

Parametrized ringdown spin expansion coefficients: A data-analysis framework for black-hole spectroscopy with multiple events

et al. 2020

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Black-hole spectroscopy is arguably the most promising tool to test gravity in extreme regimes and to probe the ultimate nature of black holes with unparalleled precision. These tests are currently limited by the lack of a ringdown parametrization that is both robust and accurate. We develop an observable-based parametrization of the ringdown of spinning black holes beyond general relativity, which we dub ParSpec (Parametrized Ringdown Spin Expansion Coefficients). This approach is perturbative in the spin, but it can be made arbitrarily precise (at least in principle) through a high-order expansion. It requires O(10) ringdown detections, which should be routinely available with the planned space mission LISA and with third-generation ground-based detectors. We provide a preliminary analysis of the projected bounds on parametrized ringdown parameters with LISA and with the Einstein Telescope, and discuss extensions of our model that can be straightforwardly included in the future. arXiv:1910.12893v1 [gr-qc] 28 Oct 2019where J = 1, 2, ..., q labels the mode; M i and χ i 1 are the detector-frame mass and spin of the i-th source, both measured assuming GR (see below); D is the order of the spin expansion; w (n) J and t (n) J are the dimensionless coefficients of the spin expansion for a Kerr BH in GR (provided in Table I for a few representative modes); γ i are dimensionless coupling constants, which can depend on the source i -see Eq. (6) below -but do not depend 1 The QNMs are identified by three integer numbers: the angular momentum number l, the azimuthal number m ∈ [−l, l], and the overtone number, which we set to zero in this paper, i.e. we only consider fundamental modes. For ease of notation we leave these indices implicit, i.e. ω (J) ≡ ω (0lm) , where J is an index that labels the mode. (n) J and δt (n) J (n) J and δt (n) J (or, equivalently, δW (n) J and δT (n) J ), these corrections depend only on the theory and not on the source.It is easy to check that, to leading order in α, the redefinitionsbring Eqs. (A1) and (A2) to the form in Eqs.(3) and (4) used in the main text. The above redefinitions also show that there is some degeneracy among the beyond-GR parameters, and that one can only constrain the combinations δw (n) J and δt (n) J , which contains the intrinsic mode corrections (δW (n) J and δT (n) J ) and the mass and spin corrections (δm and δχ).(n) J and δt (n) J are unconstrained by the data.

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“…where R 2 GB is the Gauss-Bonnet invariant 5 For a review about tests of black hole dynamics in modified theories of gravity see e.g. [38].…”

Section: Shift-symmetric Scalar-tensor Theories and Hairy Black Hmentioning

confidence: 99%

“…Note that perturbations around the black hole can be affected by the scalar even when its background is vanishing, see e.g [4,5]…”

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Black hole ringdown as a probe for dark energy

2020

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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.

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Quasinormal modes of black holes in Horndeski gravity

Cited by 93 publications

References 60 publications

Anomalous decay rate of quasinormal modes

Anomalous decay rate of quasinormal modes

Parametrized ringdown spin expansion coefficients: A data-analysis framework for black-hole spectroscopy with multiple events

Black hole ringdown as a probe for dark energy

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