Speed of gravitational waves and black hole hair

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

doi:10.1103/physrevd.97.084005

Cited by 61 publications

(62 citation statements)

References 136 publications

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“…The variant of EdGB gravity we consider is poorly constrained by weak field gravity measurements (e.g. from binary pulsars [8]), though to be consistent with the speed of gravitational waves inferred by the binary neutron star merger GW170817 [9] requires a negligible cosmological background for the dilaton field [10]. Assuming the latter, the strongest constraints on the theory may then come from gravitational wave observation of the final moments of binary black hole inspiral.…”

Section: Introductionmentioning

confidence: 72%

Scalarized black hole dynamics in Einstein-dilaton-Gauss-Bonnet gravity

Ripley

Pretorius

2020

Phys. Rev. D

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We report on a numerical investigation of the stability of scalarized black holes in Einstein dilaton Gauss-Bonnet (EdGB) gravity in the full dynamical theory, though restricted to spherical symmetry. We find evidence that for sufficiently small curvature-couplings the resulting scalarized black hole solutions are nonlinearly stable. For such small couplings, we show that an elliptic region forms inside these EdGB black hole spacetimes (prior to any curvature singularity), and give evidence that this region remains censored from asymptotic view. However, for coupling values "superextremal" relative to a given black hole mass, an elliptic region forms exterior to the horizon, implying the exterior Cauchy problem is ill-posed in this regime. *

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Section: Introductionmentioning

confidence: 72%

Scalarized black hole dynamics in Einstein-dilaton-Gauss-Bonnet gravity

Ripley

Pretorius

2020

Phys. Rev. D

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“…Indeed, we have verified that if the WKB taylor series is truncated to, for instance, second order in derivatives of the potential, one does not see the inverted behaviour in ω I ( ) as this number is not reproduced correctly. Equation (30) can be re-expressed in the following way:…”

Section: Potential Shapementioning

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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“…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%

“…As discussed, e.g., in Refs [69,82],. theories with a dimensionful coupling do not significantly affect the cosmological model, and thus the relation between cosmological distance and redshift can be assumed to be that predicted by GR.…”

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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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Speed of gravitational waves and black hole hair

Cited by 61 publications

References 136 publications

Scalarized black hole dynamics in Einstein-dilaton-Gauss-Bonnet gravity

Scalarized black hole dynamics in Einstein-dilaton-Gauss-Bonnet gravity

Anomalous decay rate of quasinormal modes

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

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