Quasi-normal modes of a massless scalar field around the 5D Ricci-flat black string

Liu, Molin; Liu, Hongya; Gui, Yuanxing

doi:10.1088/0264-9381/25/10/105001

Cited by 18 publications

(6 citation statements)

References 61 publications

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“…Second, an influent subdominant term in the asymptotic WKB expansion at spatial infinity (3.24) appears 48,49 . The higher-order WKB approach proved to be useful for finding lower overtones of the quasinormal spectrum [50][51][52][53] and is in good agreement with accurate numerical data as was shown in 54,55 . The higher-order WKB corrections lead also to better accuracy for the reflection and transmission coefficients 56 .…”

Section: Wkb Methodssupporting

confidence: 63%

Quasinormal modes of black holes: From astrophysics to string theory

2011

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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.

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Section: Wkb Methodssupporting

confidence: 63%

Quasinormal modes of black holes: From astrophysics to string theory

2011

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“…Therefore for finding the quasinormal modes and the S matrix one can use the WKB formula suggested by Schutz and Will [28] and developed to higher orders in [29]. The same formula was effectively used in a number of works for quasinormal modes of black holes [30] as well as for some scattering problems [31].…”

Section: Quasinormal Modesmentioning

confidence: 99%

Passage of radiation through wormholes of arbitrary shape

Konoplya

Zhidenko

2010

Phys. Rev. D

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We study quasinormal modes and scattering properties via calculation of the $S$-matrix for scalar and electromagnetic fields propagating in the background of spherically and axially symmetric, traversable Lorentzian wormholes of a generic shape. Such wormholes are described by the Morris-Thorne ansatz and its axially symmetric generalization. The properties of quasinormal ringing and scattering are shown to be determined by the behavior of the wormhole's shape function $b(r)$ and shift factor $\Phi(r)$ \emph{near the throat}. In particular, wormholes with the shape function $b(r)$, such that $b'(r) \approx 1$, have very long-lived quasinormal modes in the spectrum. We have proved that the axially symmetric traversable Lorentzian wormholes, unlike black holes and other compact rotating objects, do not allow for superradiance. As a by product we have shown that the 6th order WKB formula used for scattering problems of black or wormholes provides high accuracy and thus can be used for quite accurate calculations of the Hawking radiation processes around various black holes.Comment: 17 pages, the automatic procedure for calculations of the 6th order WKB quasinormal modes and reflection/transmission coefficients can be found on http://fma.if.usp.br/~konoplya/ .The procedure is authomatic and can be applied for various black and worm-holes; references adde

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“…The approximation method was extended to the third order by Iyer [46] and later to the sixth-order by Konoplya [47]. Because it is semi-analytical, the WKB method has been used in several studies on black hole QNMs [48][49][50][51]. In this section, the QNMs of higher-dimensional MP-dS black holes will be computed by the WKB approximation.…”

Section: Wkb Methodsmentioning

confidence: 99%

Massive scalar perturbations on Myers-Perry–de Sitter black holes with a single rotation

Ponglertsakul

Gwak

2020

Eur. Phys. J. C

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This study investigates the stability of higher-dimensional singly rotating Myers-Perry–de Sitter (MP–dS) black holes against scalar field perturbations. The phase spaces of MP-dS black holes with one spin parameter are discussed. Additionally, the quasinormal modes (QNMs) of MP-dS black holes are calculated via the asymptotic iteration method and sixth-order Wentzel–Kramers–Brillouin approximation. For near-extremal MP-dS black holes, the event horizon may be considerably close to the cosmological horizon. In such cases, the Pöschl–Teller technique yields an accurate analytic formula for the QNMs. It is found that when the spin parameter of a black hole increases, the scalar perturbation modes oscillate at higher frequencies and decay faster. Furthermore, the MP-dS black hole with a single rotation is found to be stable under perturbation.

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Quasi-normal modes of a massless scalar field around the 5D Ricci-flat black string

Cited by 18 publications

References 61 publications

Quasinormal modes of black holes: From astrophysics to string theory

Quasinormal modes of black holes: From astrophysics to string theory

Passage of radiation through wormholes of arbitrary shape

Massive scalar perturbations on Myers-Perry–de Sitter black holes with a single rotation

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