Ringing wormholes

Konoplya, R. A.; Molina, C.

doi:10.1103/physrevd.71.124009

Cited by 156 publications

(237 citation statements)

References 50 publications

Supporting

Mentioning

225

Contrasting

Unclassified

Order By: Relevance

“…The metric is exactly the same as the extremal Reissner-Nordström metric and the horizon is located at r = M . Classical stability of the Bocharova-Bronnikov-Melnikov-Bekenstein (BBMB) solution against the monopole perturbation has been addressed in [16][17][18]. For φ 2 > 6M…”

Section: Bocharova-bronnikov-melnikov-bekenstein Solutionmentioning

confidence: 99%

Black hole perturbation in the most general scalar-tensor theory with second-order field equations. II. The even-parity sector

2014

View full text Add to dashboard Cite

We perform a fully relativistic analysis of even-parity linear perturbations around a static and spherically symmetric solution in the most general scalar-tensor theory with second-order field equations. This paper is a sequel to Kobayashi et al. [Phys. Rev. D 85, 084025 (2012)], in which the linear perturbation analysis for the odd-parity modes is presented. Expanding the Horndeski action to second order in perturbations and eliminating auxiliary variables, we derive the quadratic action for even-parity perturbations written solely in terms of two dynamical variables. The two perturbations can be interpreted as the gravitational and scalar waves. Correspondingly, we obtain two conditions to evade ghosts and two conditions for the absence of gradient instabilities. Only one in each pair of conditions yields a new stability criterion, as the conditions derived from the stability of the gravitational-wave degree of freedom coincide with those in the odd-parity sector. Similarly, the propagation speed of one of the two modes is the same as that for the odd-parity mode, while the other differs in general from them. Our result is applicable to all the theories of gravitation with an extra single scalar degree of freedom such as the Brans-Dicke theory, f (R) models, and Galileon gravity.

show abstract

Section: Bocharova-bronnikov-melnikov-bekenstein Solutionmentioning

confidence: 99%

Black hole perturbation in the most general scalar-tensor theory with second-order field equations. II. The even-parity sector

2014

View full text Add to dashboard Cite

show abstract

“…Among important processes, the proper oscillations of higher dimensional black holes as a response to an external perturbations have been actively studied recently [3]- [16]. These oscillations are governed by the so-called quasinormal modes, which have been in the focus of gravitational research during recent years because of a few reasons.…”

Section: Introductionmentioning

confidence: 99%

Evolution of perturbations of squashed Kaluza-Klein black holes: Escape from instability

et al. 2008

View full text Add to dashboard Cite

The squashed Kaluza-Klien (KK) black holes differ from the Schwarzschild black holes with asymptotic flatness or the black strings even at energies for which the KK modes are not excited yet, so that squashed KK black holes open a window in higher dimensions. Another important feature is that the squashed KK black holes are apparently stable and, thereby, let us avoid the Gregory-Laflamme instability. In the present paper, the evolution of scalar and gravitational perturbations in time and frequency domains is considered for these squashed KK black holes. The scalar field perturbations are analyzed for general rotating squashed KK black holes. Gravitational perturbations for the so called zero mode are shown to be decayed for non-rotating black holes, in concordance with the stability of the squashed KK black holes. The correlation of quasinormal frequencies with the size of extra dimension is discussed.

show abstract

“…Recently, perturbations of more exotic objects such as wormholes, white holes, or naked singularities have been investigated. It was found that the quasinormal spectrum of Schwarzschild black holes differs from wormholes 118 and white holes 119 . Therefore, these objects, if they exist, might be detected through observations of their quasinormal ringing.…”

Section: Quasinormal Modes Of D = 4 Black Holesmentioning

confidence: 99%

Quasinormal modes of black holes: From astrophysics to string theory

2011

Self Cite

View full text Add to dashboard Cite

Perturbations of black holes, initially considered in the context of possible observations of astrophysical effects, have been studied for the past ten years in string theory, brane-world models and quantum gravity. Through the famous gauge/gravity duality, proper oscillations of perturbed black holes, called quasinormal modes (QNMs), allow for the description of the hydrodynamic regime in the dual finite temperature field theory at strong coupling, which can be used to predict the behavior of quark-gluon plasmas in the nonperturbative regime. On the other hand, the brane-world scenarios assume the existence of extra dimensions in nature, so that multidimensional black holes can be formed in a laboratory experiment. All this stimulated active research in the field of perturbations of higher-dimensional black holes and branes during recent years. In this review recent achievements on various aspects of black hole perturbations are discussed such as decoupling of variables in the perturbation equations, quasinormal modes (with special emphasis on various numerical and analytical methods of calculations), late-time tails, gravitational stability, AdS/CFT interpretation of quasinormal modes, and holographic superconductors. We also touch on state-of-the-art observational possibilities for detecting quasinormal modes of black holes.

show abstract

Ringing wormholes

Cited by 156 publications

References 50 publications

Black hole perturbation in the most general scalar-tensor theory with second-order field equations. II. The even-parity sector

Black hole perturbation in the most general scalar-tensor theory with second-order field equations. II. The even-parity sector

Evolution of perturbations of squashed Kaluza-Klein black holes: Escape from instability

Quasinormal modes of black holes: From astrophysics to string theory

Contact Info

Product

Resources

About