Quasinormal modes, scattering, and Hawking radiation in the vicinity of an Einstein-dilaton-Gauss-Bonnet black hole

Konoplya, R. A.; Zinhailo, A. F.; Stuchlík, Zdeněk

doi:10.1103/physrevd.99.124042

Cited by 106 publications

(56 citation statements)

References 90 publications

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“…Quasinormal modes and shadows of black holes are, apparently, among the most interesting characteristics of black holes in the gravitational and electromagnetic spectra. They have been observed in the modern experiments, still, leaving the wide room for interpretations and alternative theories of gravity [1][2][3][4][5][6][7][8][9][10][11]. A number of such alternative theories appeared in attempts to answer a number of fundamental questions which cannot be resolved with General Relativity, such as, for example, construction of quantum gravity or a e-mail: roman.konoplya@gmail.com (corresponding author) b e-mail: antonina.zinhailo@physics.slu.cz singularity problem.…”

Section: Introductionmentioning

confidence: 99%

Quasinormal modes, stability and shadows of a black hole in the 4D Einstein–Gauss–Bonnet gravity

2020

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Recently a D-dimensional regularization approach leading to the non-trivial $$(3+1)$$ ( 3 + 1 ) -dimensional Einstein–Gauss–Bonnet (EGB) effective description of gravity was formulated which was claimed to bypass the Lovelock’s theorem and avoid Ostrogradsky instability. Later it was shown that the regularization is possible only for some broad, but limited, class of metrics and Aoki et al. (arXiv:2005.03859) formulated a well-defined four-dimensional EGB theory, which breaks the Lorentz invariance in a theoretically consistent and observationally viable way. The black-hole solution of the first naive approach proved out to be also the exact solution of the well-defined theory. Here we calculate quasinormal modes of scalar, electromagnetic and gravitational perturbations and find the radius of shadow for spherically symmetric and asymptotically flat black holes with Gauss–Bonnet corrections. We show that the black hole is gravitationally stable when ($$-16 M^2<\alpha \lessapprox 0.6 M^2$$ - 16 M 2 < α ⪅ 0.6 M 2 ). The instability in the outer range is the eikonal one and it develops at high multipole numbers. The radius of the shadow $$R_{Sh}$$ R Sh obeys the linear law with a remarkable accuracy.

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Section: Introductionmentioning

confidence: 99%

Quasinormal modes, stability and shadows of a black hole in the 4D Einstein–Gauss–Bonnet gravity

2020

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“…Furthermore, we apply the geometrical optics approximation and assume the emitted massless quanta move along null geodesics. However, to get a precise lifetime one has to compute the grey body factors of all the particles [46][47][48][49][50][51][52][53][54][55][56][57][58][59][60][61][62][63]. On the other hand, near the end of the evaporation, effective field theory starts to fail, and quantum gravity effect may stop the evaporation, leaving a black hole "remnant" [64][65][66][67].…”

Section: Summary and Discussionmentioning

confidence: 99%

Black hole evaporation in Lovelock gravity with diverse dimensions

Yung

2019

Physics Letters B

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We investigate the black hole evaporation process in Lovelock gravity with diverse dimensions. By selecting the appropriate coefficients, the space-time solutions can possess a unique AdS vacuum with a fixed cosmological constant Λ = − (d−1)(d−2) 2ℓ 2 . The black hole solutions can be divided into two cases: d > 2k + 1 and d = 2k + 1. In the case of d > 2k + 1, the black hole is in an analogy with the Schwarzschild AdS black hole, and the life time is bounded by a time of the order of ℓ d−2k+1 , which reduces Page's result on the Einstein gravity in k = 1. In the case of d = 2k + 1, the black hole resembles the three dimensional black hole. The black hole vacuum corresponds to T = 0, so the black hole will take infinite time to evaporate away for any initial states, which obeys the third law of thermodynamics. In the asymptotically flat limit ℓ → ∞, the system reduces to the pure Lovelock gravity that only possesses the highest k-th order term. For an initial mass M0, the life time of the black hole is in the order of M d−2k+1 d−2k−1 0 .

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“…This approach was used to construct the analytical approximation of numerical blackhole solutions in the Einstein-Weyl [16], Einstein-dilaton-Gauss-Bonnet [17] and Einstein-scalar-Maxwell [18] theories. Further studies of observables in these parametrized spacetimes [19][20][21][22][23][24] showed that usually it is sufficient only two-three orders of the continued fraction expansion in order to achieve reasonable accuracy.…”

Section: Introductionmentioning

confidence: 99%

Einstein-scalar–Gauss-Bonnet black holes: Analytical approximation for the metric and applications to calculations of shadows

Konoplya¹,

Παππάς²,

Zhidenko³

2020

Phys. Rev. D

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Recently, numerical solutions to the field equations of Einstein-scalar-Gauss-Bonnet (EsGB) gravity that correspond to black-holes with non-trivial scalar hair have been reported. Here, we employ the method of the continued-faction expansion in terms of a compact coordinate in order to obtain an analytical approximation for the aforementioned solutions. For a wide variety of coupling functions to the Gauss-Bonnet term we were able to obtain analytical expressions for the metric functions and the scalar field. In addition we estimated the accuracy of these approximations by calculating the black-hole shadows for such black holes. Excellent agreement between the numerical solutions and analytical approximations has been found.

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Quasinormal modes, scattering, and Hawking radiation in the vicinity of an Einstein-dilaton-Gauss-Bonnet black hole

Cited by 106 publications

References 90 publications

Quasinormal modes, stability and shadows of a black hole in the 4D Einstein–Gauss–Bonnet gravity

Quasinormal modes, stability and shadows of a black hole in the 4D Einstein–Gauss–Bonnet gravity

Black hole evaporation in Lovelock gravity with diverse dimensions

Einstein-scalar–Gauss-Bonnet black holes: Analytical approximation for the metric and applications to calculations of shadows

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