Dynamical Formation of Kerr Black Holes with Synchronized Hair: An Analytic Model

Herdeiro, Carlos; Radu, Eugen

doi:10.1103/physrevlett.119.261101

Cited by 82 publications

(89 citation statements)

References 54 publications

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“…Something similar occurs in other scenarios, such as in scalar field theories, where the conditions to yield identical background solutions and linear perturbations are very special [70,71]. Thus, a dedicated analysis of the perturbation equations for gravitational waves and their phenomenological implications should be carried out for each gravity theory that generates the line element (3).…”

Section: Phenomenological Implicationsmentioning

confidence: 92%

Absorption by black hole remnants in metric-affine gravity

et al. 2019

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Using numerical methods, we investigate the absorption properties of a family of nonsingular solutions which arise in different metric-affine theories, such as quadratic and Born-Infeld gravity. These solutions continuously interpolate between Schwarzschild black holes and naked solitons with wormhole topology. The resulting spectrum is characterized by a series of quasibound states excitations, associated with the existence of a stable photonsphere.

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Section: Phenomenological Implicationsmentioning

confidence: 92%

Absorption by black hole remnants in metric-affine gravity

et al. 2019

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“…How much energy can be extracted from the Kerr BH region into the hair? Fully non-linear numerical evolutions of the superradiant instability of a Kerr BH triggered by a complex vector field were performed in [25], leading to the formation of that BH with synchronised (vector) hair [26], first discussed in [27]. These simulations showed that the maximal energy extracted was ∼ 0.09M of the original BH with mass M .…”

Section: The Hair Formation and Hair Instability Timescalesmentioning

confidence: 99%

EHT Constraint on the Ultralight Scalar Hair of the M87 Supermassive Black Hole

2019

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Hypothetical ultralight bosonic fields will spontaneously form macroscopic bosonic halos around Kerr black holes, via superradiance, transferring part of the mass and angular momentum of the black hole into the halo. Such process, however, is only efficient if resonant: when the Compton wavelength of the field approximately matches the gravitational scale of the black hole. For a complex-valued field, the process can form a stationary, bosonic field-black hole equilibrium state -a black hole with synchronised hair. For sufficiently massive black holes, such as the one at the centre of the M87 supergiant elliptic galaxy, the hairy black hole can be robust against its own superradiant instabilities, within a Hubble time. Studying the shadows of such scalar hairy black holes, we constrain the amount of hair which is compatible with the Event Horizon Telescope (EHT) observations of the M87 supermassive black hole, assuming the hair is a condensate of ultralight scalar particles of mass µ ∼ 10 −20 eV, as to be dynamically viable. We show the EHT observations set a weak constraint, in the sense that typical hairy black holes that could develop their hair dynamically, are compatible with the observations, when taking into account the EHT error bars and the black hole mass/distance uncertainty.

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“…Recently, however, Frolov et al [35] (henceforth FKKS), have found an ansatz, based on the conformal Killing-Yano 2-form, which separates the Proca quasi-normal mode equations on the Kerr-NUT-(A)dS family of spacetimes. We use this approach here, in which finding the spectrum of Proca modes reduces to solving two decoupled, differential eigenvalue problems, to systematically cover the parameter space of superradiantly bility [15,22,23], though these will still be unstable to higher m superradiant modes [24]. unstable modes.…”

Section: Introductionmentioning

confidence: 99%

Gravitational wave signatures of ultralight vector bosons from black hole superradiance

Siemonsen

East

2020

Phys. Rev. D

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In the presence of an ultralight bosonic field, spinning black holes are unstable to superradiance. The rotational energy of the black hole is converted into a non-axisymmetric, oscillating boson cloud which dissipates through the emission of nearly monochromatic gravitational radiation. Thus, gravitational wave observations by ground-or space-based detectors can be used to probe the existence of dark particles weakly coupled to the Standard Model. In this work, we focus on massive vector bosons, which grow much faster through superradiance, and produce significantly stronger gravitational waves compared to the scalar case. We use techniques from black hole perturbation theory to compute the relativistically-correct gravitational wave signal across the parameter space of different boson masses and black holes masses and spins. This fills in a gap in the literature between flatspace approximations, which underestimate the gravitational wave amplitude in the non-relativistic limit, and overestimate it in the relativistic regime, and time-domain calculations, which have only covered a limited part of the parameter space. We also identify parameter ranges where overtone superradiantly unstable modes will grow faster than the lower frequency fundamental modes. Such cases will produce a distinct gravitational wave signal due to the beating of the simultaneously populated modes, which we compute.1 An even set of minimally coupled bosonic fields can be arranged to form an axisymmetric energy-momentum distribution, and hence a stationary hairy BH at the saturation point of the insta-arXiv:1910.09476v1 [gr-qc]

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Dynamical Formation of Kerr Black Holes with Synchronized Hair: An Analytic Model

Cited by 82 publications

References 54 publications

Absorption by black hole remnants in metric-affine gravity

Absorption by black hole remnants in metric-affine gravity

EHT Constraint on the Ultralight Scalar Hair of the M87 Supermassive Black Hole

Gravitational wave signatures of ultralight vector bosons from black hole superradiance

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