Imprints of dark matter on gravitational ringing of supermassive black holes

Zhang, Chao; Zhu, Tao; Fang, Xiongjun; Wang, Anzhong

doi:10.1016/j.dark.2022.101078

Cited by 17 publications

(4 citation statements)

References 62 publications

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“…Note that here, is the metric function mentioned in [38], rather than the cosmological constant. Then, the master variable can be constructed as…”

Section: Bardeen (Anti-) De Sitter Black Holementioning

confidence: 99%

Quasinormal modes and isospectrality of Bardeen (Anti-) de Sitter black holes*

Zhao 赵,

Liu 刘,

Zhang 张

et al. 2024

Chinese Phys. C

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Black holes (BHs) exhibiting coordinate singularities but lacking essential singularities throughout the entire spacetime are referred to as regular black holes (RBHs). The initial formulation of RBHs was presented by Bardeen, who considered the Einstein equation coupled with a nonlinear electromagnetic field. In this study, we investigate the gravitational perturbations, including the axial and polar sectors, of the Bardeen (Anti-) de Sitter black holes. We derive the master equations with source terms for both axial and polar perturbations, and subsequently compute the quasinormal modes (QNMs) through numerical methods. For the Bardeen de Sitter black hole, we employ the 6th-order WKB approach. The numerical results reveal that the isospectrality is broken in this case. Conversely, for Bardeen Anti-de Sitter black holes, the QNM frequencies are calculated by using the HH method.

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“…Note that here, is the metric function mentioned in [38], rather than the cosmological constant. Then, the master variable can be constructed as…”

Section: Bardeen (Anti-) De Sitter Black Holementioning

confidence: 99%

Quasinormal modes and isospectrality of Bardeen (Anti-) de Sitter black holes*

Zhao 赵,

Liu 刘,

Zhang 张

et al. 2024

Chinese Phys. C

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“…The interaction of a black hole binary and a scalar field environment in the early-inspiral regime, where the separation is large and almost constant with time, has been explored via effective field theory [110,111], weak field approximations [112][113][114][115][116][117][118][119][120]; perturbative schemes [100,102,[121][122][123][124][125][126], and N-body and mesh numerical simulations [29,80,[127][128][129]. The effect of a non-vacuum environment on the post-merger "ringdown" regime, particularly the effect on the frequencies of the characteristic quasi-normal modes has also been explored by a number of authors [130][131][132][133][134]. To model the highly relativistic and dynamical merger one must use full numerical relativity.…”

Section: Introductionmentioning

confidence: 99%

Black hole merger simulations in wave dark matter environments

et al. 2023

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The interaction of binary black hole mergers with their environments can be studied using numerical relativity simulations. These start only a short finite time before merger, at which point appropriate initial conditions must be imposed. A key task is therefore to identify the configuration that is appropriate for the binary and its environment at this stage of the evolution. In this work we study the behaviour of wave dark matter around equal mass black hole binaries, finding that there is a preferred, quasi-stationary profile that persists and grows over multiple orbits, in contrast to heavier mass dark matter where any overdensity tends to be dispersed by the binary motion. Whilst different initial configurations converge to the preferred quasi-stationary one after several orbits, unwanted transient oscillations are generated in the process, which may impact on the signal in short simulation runs. We also point out that naively superimposing the matter onto a circular binary results in artificially eccentric orbits due to the matter backreaction, which is an effect of the initial conditions and not a signature of dark matter. We discuss the further work required so that comparison of waveforms obtained with environments to vacuum cases can be done in a meaningful way.

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“…These features indicate that the method is a promising alternative in the toolkit for black hole QNMs. The method matrix method is shown to offer reasonable accuracy as well as efficiency, and has been adopted in various studies [30,[61][62][63][64][65][66][67][68][69][70][71][72][73]. Nonetheless, it also entails some drawbacks.…”

Section: Introductionmentioning

confidence: 99%

High-order matrix method with delimited expansion domain

Lin

Qian

2023

Class. Quantum Grav.

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Motivated by the substantial instability of the fundamental and high-overtone quasinormal modes, recent developments regarding the notion of black hole pseudospectrum call for numerical results with unprecedented precision.This work generalizes and improves the matrix method for black hole quasinormal modes to higher orders, specifically aiming at a class of perturbations to the metric featured by discontinuity intimately associated with the quasinormal mode structural instability.The approach is based on the mock-Chebyshev grid, which guarantees its convergence in the degree of the interpolant.In practice, solving for black hole quasinormal modes is a formidable task.The presence of discontinuity poses a further difficulty so that many well-known approaches cannot be employed straightforwardly.Compared with other viable methods, the modified matrix method is competent in speed and accuracy. Therefore, the method serves as a helpful gadget for relevant studies.

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Imprints of dark matter on gravitational ringing of supermassive black holes

Cited by 17 publications

References 62 publications

Quasinormal modes and isospectrality of Bardeen (Anti-) de Sitter black holes*

Quasinormal modes and isospectrality of Bardeen (Anti-) de Sitter black holes*

Black hole merger simulations in wave dark matter environments

High-order matrix method with delimited expansion domain

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