Implications of the quantum nature of the black hole horizon on the gravitational-wave ringdown

Chakraborty, Sumanta; Maggio, Elisa; Mazumdar, Anupam; Pani, Paolo

doi:10.48550/arxiv.2202.09111

Cited by 8 publications

(10 citation statements)

References 62 publications

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“…Though the resultsby and large -are consistent with that of a general relativistic black hole, there is room for alternatives [12][13][14][15][16][17][18]. In particular, if stellar structures can exist within the region between the black hole horizon and the photon sphere, the gravitational wave signal, within the current experimental errors, will very much look like that of a general relativistic black hole [19][20][21][22][23][24][25][26]. Therefore, the existence of such stellar structures and study of their physical properties are always encouraging in its own right.…”

Section: Introductionmentioning

confidence: 62%

Universality of the Buchdahl sphere

Chakraborty¹,

Dadhich²

2022

Preprint

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Buchdahl sphere, the limiting stable isotropic stellar structure without exotic matter, plays a very important role, as far as the near horizon physics is concerned. This is because, the radius of the Buchdahl sphere lies between the horizon and the photon sphere, such that the signal arising from gravitational wave and black hole shadow will mimic that of a black hole. Here, we show certain universal properties associated with the Buchdahl sphere, in the sense that these properties will not change even if electric charge is included in the stellar structure. Moreover, these universal properties transcend general relativity and holds good in pure Lovelock theories of gravity as well. Using these universalities, we have proposed a Buchdahl limit for rotating stellar configuration. Finally, the universality of the Buchdahl limit in terms of the gravitational and non-gravitational field energies and also in terms of the photon sphere is also discussed.

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Section: Introductionmentioning

confidence: 62%

Universality of the Buchdahl sphere

Chakraborty¹,

Dadhich²

2022

Preprint

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“…Contrary to the common lore that detections of echoes in late-time ringdown signals can be used to distinguish black holes with wormholes, echo signals have been reported in several black hole models, e.g., quantum black holes [38][39][40][41][42], black holes with discontinuous effective potentials [43],…”

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confidence: 85%

Echoes from Hairy Black Holes

Guo,

Wang,

et al. 2022

Preprint

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We study the waveforms of time signals produced by scalar perturbations in static hairy black holes, in which the perturbations can be governed by a double-peak effective potential.The inner potential peak would give rise to echoes, which provide a powerful tool to test the Kerr hypothesis. The waveforms are constructed in the time and frequency domains, and we find that the late-time waveforms are determined by the long-lived and sub-long-lived quasinormal modes, which are trapped in the potential valley and near the smaller peak, respectively. When the distance between the peaks is significantly larger than the width of the peaks, a train of decaying echo pulses is produced by the superposition of the long-lived and sub-long-lived modes. In certain cases, the echoes can vanish and then reappear. When the peaks are close enough, one detects far fewer echo signals and a following sinusoid tail, which is controlled by the long-lived or sub-long-lived mode and hence decays very slowly.

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“…Delayed and repeating gravitational wave echoes emitted by compact-binary mergers [1][2][3], following the main gravitational waves (GWs), can be signatures of: (i) deviations of laws of gravity from general relativity [4], (ii) near-horizon quantum structures surrounding black holes (BHs) [5][6][7][8][9][10][11][12], and (iii) the absence of event horizon, namely the existence of horizonless Exotic Compact Objects (ECOs) [13][14][15][16][17]. We must emphasize that strong arguments (within the context of general relativity and standard model of matter) exist against the existence of echoes and ECOs, including: (i) the ergoregion instability [18][19][20][21], (ii) the formation of a trapped surface due to the pileup of energy near the stable photon orbit [22][23][24], (iii) the collapse of ECO due to the gravity of incident GWs [25,26], and (iv) other nonlinear effects [27].…”

Section: Introductionmentioning

confidence: 99%

“…[36] estimated the contribution of GW echoes to stochastic background. In terms of the membrane diagram, Maggio et al [37] and Chakraborty et al [12] treated the ECO surface as a dissipative fluid, and related the reflectivity to the bulk and the shear viscosity. More recently, the echoes of fuzzballs [38,39] were computed numerically in Ref.…”

Section: Introductionmentioning

confidence: 99%

Gravitational-wave echoes from numerical-relativity waveforms via space-time construction near merging compact objects

Ma,

Wang,

Deppe

et al. 2022

Preprint

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We propose a new approach toward reconstructing the late-time near-horizon geometry of merging binary black holes, and toward computing gravitational-wave echoes from exotic compact objects. A binary black-hole merger spacetime can be divided by a time-like hypersurface into a Black-Hole Perturbation (BHP) region, in which the space-time geometry can be approximated by homogeneous linear perturbations of the final Kerr black hole, and a nonlinear region. At late times, the boundary between the two regions is an infalling shell. The BHP region contains late-time gravitational-waves emitted toward the future horizon, as well as those emitted toward future null infinity. In this region, by imposing no-ingoing wave conditions at past null infinity, and matching out-going waves at future null infinity with waveforms computed from numerical relativity, we can obtain waves that travel toward the future horizon. In particular, the Newman-Penrose ψ 0 associated with the in-going wave on the horizon is related to tidal deformations measured by fiducial observers floating above the horizon. We further determine the boundary of the BHP region on the future horizon by imposing that ψ 0 inside the BHP region can be faithfully represented by quasi-normal modes. Using a physically-motivated way to impose boundary conditions near the horizon, and applying the so-called Boltzmann reflectivity, we compute the quasi-normal modes of non-rotating ECOs, as well as gravitational-wave echoes. We also investigate the detectability of these echoes in current and future detectors, and prospects for parameter estimation.

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Implications of the quantum nature of the black hole horizon on the gravitational-wave ringdown

Cited by 8 publications

References 62 publications

Universality of the Buchdahl sphere

Universality of the Buchdahl sphere

Echoes from Hairy Black Holes

Gravitational-wave echoes from numerical-relativity waveforms via space-time construction near merging compact objects

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