Quasinormal Modes Beyond Kerr

Zimmerman, Aaron; Yang, Huan; Mark, Z.; Chen, Yanbei; Lehner, Luis

doi:10.1007/978-3-319-10488-1_19

Cited by 21 publications

(14 citation statements)

References 11 publications

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“…In order to solve the above equation and obtain the frequency shift δω, we shall apply a technique that Mark, Yang, Zimmerman, and Chen first developed for studying perturbations to Kerr-Newman black holes [44,45] and was later applied to near-extremal black holes to investigate turbulent-like instabilities [46]. In particular, these studies have verified the validity of this method under a variety of different scenarios.…”

Section: A Perturbative Methods For Solving Coupled Wave Equationsmentioning

confidence: 99%

Stability of force-free magnetospheres

Yang

Zhang

2014

Phys. Rev. D

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We analyze the dynamical evolution of a perturbed force-free magnetosphere of a rotating black hole, which is described by the Blandford-Znajek solution in the stationary limit. We find that the electromagnetic field perturbations can be classified into two categories: "trapped modes" and "traveling waves". The trapped modes are analogous to the vacuum (without plasma) electromagnetic quasinormal modes in rotating black hole spacetimes, but with different eigenfrequencies and wave functions, due to their coupling with the background electromagnetic field and current. The traveling waves propagate freely to infinity or the black hole horizon along specific null directions, and they are closely related to the no-scattering Poynting flux solutions discovered by Brennan, Gralla and Jacobson. Our results suggest that the Blandford-Znajek solution is mode stable, and more importantly we expect this study to illuminate the dynamical behavior of force-free magnetospheres as well as to shed light on the path to new exact solutions.

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Section: A Perturbative Methods For Solving Coupled Wave Equationsmentioning

confidence: 99%

Stability of force-free magnetospheres

Yang

Zhang

2014

Phys. Rev. D

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“…For example, in Paper I we showed that slowly rotating Kerr BHs can be accommodated within the formalism. Recent work on higher-derivative corrections to the Kerr geometry [76] and on QNM frequencies of rotating solutions for small coupling [53,54] may allow us to make progress on the calculation of QNMs in modified gravity for rotating BH remnants, such as those observed by the LIGO/Virgo collaboration [77]. Related attempts at parametrizing deviations from the Kerr QNM spectrum [78,79] made use of the connection between the stability of null geodesics and QNMs [80][81][82].…”

Section: Conclusion and A Computational Recipementioning

confidence: 99%

“…Even if GR is the correct theory of gravity, matter fields can couple with each other, and the perturbations of these fields will in general be coupled. This happens, for instance, in the Einstein-Maxwell system [49][50][51][52][53][54][55] or for axionic fields in charged BH backgrounds [10,[56][57][58].…”

Section: Introductionmentioning

confidence: 99%

Parametrized black hole quasinormal ringdown. II. Coupled equations and quadratic corrections for nonrotating black holes

et al. 2019

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Linear perturbations of spherically symmetric spacetimes in general relativity are described by radial wave equations, with potentials that depend on the spin of the perturbing field. In previous work [1] we studied the quasinormal mode spectrum of spacetimes for which the radial potentials are slightly modified from their general relativistic form, writing generic small modifications as a power-series expansion in the radial coordinate. We assumed that the perturbations in the quasinormal frequencies are linear in some perturbative parameter, and that there is no coupling between the perturbation equations. In general, matter fields and modifications to the gravitational field equations lead to coupled wave equations. Here we extend our previous analysis in two important ways: we study second-order corrections in the perturbative parameter, and we address the more complex (and realistic) case of coupled wave equations. We highlight the special nature of coupling-induced corrections when two of the wave equations have degenerate spectra, and we provide a ready-to-use recipe to compute quasinormal modes. We illustrate the power of our parametrization by applying it to various examples, including dynamical Chern-Simons gravity, Horndeski gravity and an effective field theory-inspired model. arXiv:1906.05155v3 [gr-qc]

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“…The EVP method makes use of an original technique for applying perturbation theory to zeroth order solutions which are not square-integrable. This method can be (and recently has been [22][23][24]) applied to other problems in theoretical physics.…”

Section: Introductionmentioning

confidence: 99%

Quasinormal modes of weakly charged Kerr-Newman spacetimes

et al. 2015

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The resonant mode spectrum of the Kerr-Newman spacetime is presently unknown. These modes, called the quasinormal modes, play a central role in determining the stability of Kerr-Newman black holes and their response to perturbations. We present a new formalism, generalized from time-independent perturbation theory in quantum mechanics, for calculating the quasinormal mode frequencies of weakly charged Kerr-Newman spacetimes of arbitrary spin. Our method makes use of an original technique for applying perturbation theory to zeroth-order solutions that are not square-integrable, and it can be applied to other problems in theoretical physics. The new formalism reveals no unstable modes, which together with previous results in the slow-rotation limit strongly indicates the modal stability of the Kerr-Newman spacetime. Our techniques and results are of interest in the areas of holographic duality, foundational problems in general relativity, and possibly in astrophysical systems.

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Quasinormal Modes Beyond Kerr

Cited by 21 publications

References 11 publications

Stability of force-free magnetospheres

Stability of force-free magnetospheres

Parametrized black hole quasinormal ringdown. II. Coupled equations and quadratic corrections for nonrotating black holes

Quasinormal modes of weakly charged Kerr-Newman spacetimes

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