Scalar Hairy Black Holes in Four Dimensions are Unstable

Ganchev, Bogdan; Santos, Jorge E.

doi:10.1103/physrevlett.120.171101

Cited by 41 publications

(40 citation statements)

References 47 publications

(67 reference statements)

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“…It is worth to point out that it is difficult to numerical analysis the stability properties of rotating multistate boson stars. However, a good way to guarantee the stability of a specific solution is to have the linear perturbation mode in [39].…”

Section: Discussionmentioning

confidence: 99%

Rotating multistate boson stars

Sun

et al. 2020

Phys. Rev. D

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In this paper we construct the rotating boson stars composed of the coexisting states of two scalar fields, including the ground and first excited states. We show that the coexisting phase with both the ground and first excited states for rotating multistate boson stars (RMSBS). In contrast to the solutions of the nodeless boson stars, the rotating boson stars with two states have two types of nodes, including the 1 S 2 S state and the 1 S 2 P state. Moreover, we explore the properties of the mass M of rotating boson stars with two states as a function the synchronized frequency ω, as well as the non-synchronized frequency ω 2 . Finally, we also study the dependence of the mass M of rotating boson stars with two states on angular momentum for both the synchronized frequency ω and the non-synchronized frequency ω 2 . a

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Section: Discussionmentioning

confidence: 99%

Rotating multistate boson stars

Sun

et al. 2020

Phys. Rev. D

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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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“…The uniqueness theorem [30][31][32][33][34][35][36] tells us that curved spacetime described by Kerr-Newman(KN) metric in the Einstein-Maxwell gravitational theory can hold at most three global conserved quantities, which are named as mass, electric charge and angular momentum. Correspondingly, no-hair conjecture [19,25,[37][38][39][40][41][42] for black holes states that static matter field (such as the massless scalar field) perturbations of the black hole in KN family can not be permanently hold.…”

Section: Introductionmentioning

confidence: 99%

The fastest relaxation rate of higher-dimensional Reissner–Nordström black hole

2019

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In the eikonal regime, we analytically calculate quasinormal resonance frequencies for massless scalar perturbations of the higher-dimensional Reissner-Nordström (RN) black holes. Remarkably, we find that the higher-dimensional RN black holes coupled with the massless scalar fields have the fastest relaxation rates in the Schwarzschild limit, this is qualitatively different from the fourdimensional case where the black hole with non-vanishing charge has the fastest relaxation rate. arXiv:1909.08562v2 [gr-qc]

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Scalar Hairy Black Holes in Four Dimensions are Unstable

Cited by 41 publications

References 47 publications

Rotating multistate boson stars

Rotating multistate boson stars

Gravitational wave signatures of ultralight vector bosons from black hole superradiance

The fastest relaxation rate of higher-dimensional Reissner–Nordström black hole

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