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

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

doi:10.48550/arxiv.2003.01188

Cited by 68 publications

(99 citation statements)

References 48 publications

(63 reference statements)

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“…The Regge-Wheeler and Zerilli equations are isospectral and this can be made explicit by performing a Darboux transformation, known in this context as the Chandrasekhar transformation, that relates them [73]. We extend this transformation here to linear order in spin in order to connect V −GR lm and V +GR lm in (44) and (48), respectively. Explicitly, we wish to transform…”

Section: Appendix B: Integrals Of Associated Legendre Functionsmentioning

confidence: 99%

“…The corrections to the QNM frequencies of nonrotating black holes have been obtained in a number of theories, including dynamical Chern-Simons gravity [38,39], Einstein-dilaton-Gauss-Bonnet gravity [40,41], and theories with quartic [33,42] and cubic [18] curvature terms, among other models [43][44][45][46]. In addition, theoryindependent approaches were studied in [42,47,48], while eikonal QNMs beyond GR were investigated in [49][50][51].…”

Section: Introductionmentioning

confidence: 99%

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Ringing of rotating black holes in higher-derivative gravity

2020

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We compute scalar quasinormal mode (QNM) frequencies in rotating black hole solutions of the most general class of higher-derivative gravity theories, to quartic order in the curvature, that reduce to General Relativity for weak fields and are compatible with its symmetries. The wave operator governing the QNMs is not separable, but we show one can extract the QNM frequencies by a projection onto the set of spheroidal harmonics. We have obtained accurate results for the quasinormal frequency corrections relative to Kerr for rotating black holes with dimensionless spins up to ∼ 0.7. We also discuss to what extent our results carry over to the phenomenologically more relevant case of gravitational QNMs. Finally we provide an ancillary computational package that allows one to generalize our calculations to any effective energy-momentum tensor arising from higher-derivative terms in the effective action.

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Section: Appendix B: Integrals Of Associated Legendre Functionsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Ringing of rotating black holes in higher-derivative gravity

2020

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“…Therefore, it is very safe to consider test fields in the background of these black holes using the same regularization scheme. Along this spirit, the Einstein-Gauss-Bonnet gravity in the 4D spacetime has been investigated extensively on various aspects [19][20][21][22][23][24][25][26][27][28][29][30][31][32][33][34][35][36][37][38].…”

Section: Introductionmentioning

confidence: 99%

Tidal effects in 4D Einstein-Gauss-Bonnet Black Hole Spacetime

Li,

Chen,

Jing

2021

Preprint

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We have investigated tidal forces and geodesic deviation motion in the 4D-Einstein-Gauss-Bonnet spacetime. Our results show that tidal force and geodesic deviation motion depend sharply on the sign of Gauss-Bonnet coupling constant. Comparing with Schwarzschild spacetime, the strength of tidal force becomes stronger for the negative Gauss-Bonnet coupling constant, but is weaker for the positive one. Moreover, tidal force behaves like those in the Schwarzschild spacetime as the coupling constant is negative, and like those in Reissner-Nordström black hole as the constant is positive.We also present the change of geodesic deviation vector with Gauss-Bonnet coupling constant under two kinds of initial conditions.

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“…The shadow size of the GB black hole was also investigated in Refs. [28,29]. The negative GB coupling enlarges the shadow, while the positive one shrinks it [29].…”

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confidence: 98%

“…A non-trivial and novel four-dimensional static and spherically symmetric black hole solution was obtained [27]. The quasinormal modes of the solution were examined in [28], where the result shows that the damping rate is more sensitive than the real part by varying the GB coupling parameter. The shadow size of the GB black hole was also investigated in Refs.…”

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confidence: 99%

Extended thermodynamics and microstructures of four-dimensional charged Gauss-Bonnet black hole in AdS space

Wei,

Liu

2020

Preprint

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The discovery of new four-dimensional black hole solutions presents a new approach to understand the Gauss-Bonnet gravity in low dimensions. In this paper, we test the Gauss-Bonnet gravity by studying the phase transition and microstructures for the four-dimensional charged AdS black hole. In the extended phase space, where the cosmological constant and the Gauss-Bonnet coupling parameter are treated as thermodynamic variables, we find that the thermodynamic first law and the corresponding Smarr formula are satisfied. Both in the canonical ensemble and grand canonical ensemble, we observe the small-large black hole phase transition, which is similar to the case of the van der Walls fluid. This phase transition can also appear in the neutral black hole system. Furthermore, we construct the Ruppeiner geometry, and find that besides the attractive interaction, the repulsive interaction can also dominate among the microstructures for the small black hole with high temperature in a charged or neutral black hole system. This is quite different from the fivedimensional neutral black hole, for which only dominant attractive interaction can be found. The critical behaviors of the normalized scalar curvature are also examined. These results will shed new light into the characteristic property of four-dimensional Gauss-Bonnet gravity.

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

Cited by 68 publications

References 48 publications

Ringing of rotating black holes in higher-derivative gravity

Ringing of rotating black holes in higher-derivative gravity

Tidal effects in 4D Einstein-Gauss-Bonnet Black Hole Spacetime

Extended thermodynamics and microstructures of four-dimensional charged Gauss-Bonnet black hole in AdS space

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