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 gravity wormholes sourced by a phantom scalar field

Karakasis, Thanasis; Papantonopoulos, Eleftherios; Vlachos, Christoforos

doi:10.1103/physrevd.105.024006

Cited by 30 publications

(6 citation statements)

References 104 publications

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“…This feature has lead the search and analysis of QNM to be an important subject in the gravitationalwave literature. Hence, one can use gravitational-wave observations in order to test general relativity, examining for instance the validity of the "no-hair theorem" [74][75][76], and use the predictions of QNM properties to constrain and classify modified gravity theories [77][78][79][80][81][82][83][84][85]. Furthermore, the QNM frequency can also partly reveal the stability of spacetime geometry under small perturbations [86,87].…”

Section: Introductionmentioning

confidence: 99%

Quasinormal modes of black holes in f(T) gravity

Zhao¹,

Ren²,

Ilyas³

et al. 2022

Preprint

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We calculate the quasinormal modes (QNM) frequencies of a test massless scalar field around static black holes in f (T ) gravity. Focusing on quadratic f (T ) modifications, which is a good approximation for every realistic f (T ) theory, we first extract the spherically symmetric solutions using the perturbative method, imposing two ansätze for the metric functions, which suitably quantify the deviation from the Schwarzschild solution. Moreover, we extract the effective potential and then we calculate the QNM frequency of the obtained solutions. Firstly, we solve the Schrödinger-like equation numerically using the discretization method, and we extract the frequency and the time evolution of the dominant mode applying the function fit method. Secondly, we perform a semianalytical calculation by applying the third-order WKB approximation method. We show that the results for f (T ) gravity are different comparing to General Relativity, and in particular we obtain a different slope and period of the field decay behavior for different values of the model parameter. Hence, under the light of gravitational-wave observations of increasing accuracy from binary systems, the whole analysis could be used as an additional tool in order to test General Relativity and examine whether torsional gravitational modifications are possible.

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Section: Introductionmentioning

confidence: 99%

Quasinormal modes of black holes in f(T) gravity

Zhao¹,

Ren²,

Ilyas³

et al. 2022

Preprint

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“…A number of dark energy cosmological models without the cosmological constant have been proposed to explain cosmic acceleration. There are a quintessence (canonical scalar field) [3][4][5], a phantom (non-canonical scalar field) [6][7][8], fermion fields [9][10][11][12], tachyon fields [13,14], Chaplygin gas with a special equation of state (EoS) [15,16] and so on. All these models have been successfully investigated in the framework of Riemannian gravitational theories with a Levi-Civita connection, where space-time is mediated by curvature in general relativity (GR).…”

Section: Introductionmentioning

confidence: 99%

f(T, B) gravity with statistically fitting of H(z)

Shekh¹,

Myrzakulov

Bouali

et al. 2023

Commun. Theor. Phys.

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Some recent developments (accelerated expansion) in the universe cannot be explained by the conventional formulation of general relativity. We applied the recently proposed $f(T,B)$ gravity to investigate the accelerated expansion of the universe. By parametrizing the Hubble parameter and estimating the best fit values of the model parameters $b_{0}$, $b_{1}$, and $b_{2}$ imposed from Supernovae type Ia, Cosmic Microwave Background, Baryon Acoustic Oscillation, and Hubble data using the Markov Chain Monte Carlo (MCMC) method, we propose a method to determine the precise solutions to the field equations. We then observed that the model appears to be in good agreement with the observations. A change from the deceleration to the acceleration phase of the universe is shown by the evolution of the deceleration parameter. In addition, we investigate the behavior of statefinder analysis, equation of state (EoS) parameters along with the energy conditions. Further, to discuss other cosmological parameters, we consider some well-known $f (T,B)$ gravity model, specifically, $f(T,B)=a T^b+c B^d$. Lastly, we found that the considered $f (T,B)$ gravity models predict that the present Universe is accelerating and the EoS parameter behaves like the $\Lambda$CDM model.

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“…For horizonless compact objects, there could be echoes in the ringdown signal, which is the smoking gun for the existence of the horizonless compact objects [15,22,36]. One can also use the QNMs to constrain modified gravity theories [37][38][39][40][41][42][43][44][45]. It has also been found that the QNM spectrum is unstable under a small perturbation of the potential [46,47].…”

Section: Introductionmentioning

confidence: 99%

Quasinormal Modes of a Charged Black Hole with Scalar Hair

Guo

Tan

2023

Universe

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Based on the five-dimensional Einstein–Maxwell theory, Bah et al. constructed a singularity-free topology star/black hole [Phys. Rev. Lett. 126, 151101 (2021)]. After performing the Kaluza–Klein reduction, i.e., integrating the extra space dimension, it can obtain an effective four-dimensional spherically static charged black hole with scalar hair. In this paper, we study the quasinormal modes (QNMs) of the scalar, electromagnetic, and gravitational fields in the background of this effective four-dimensional charged black hole. The radial parts of the perturbed fields all satisfy a Schrödinger-like equation. Using the asymptotic iteration method, we obtain the QNM frequencies semianalytically. For low-overtone QNMs, the results obtained using both the asymptotic iteration method and the Wentzel–Kramers–Brillouin approximation method agree well. In the null coordinates, the evolution of a Gaussian package is also studied. The QNM frequencies obtained by fitting the evolution data also agree well with the results obtained using the asymptotic iteration method.

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f(R) gravity wormholes sourced by a phantom scalar field

Cited by 30 publications

References 104 publications

Quasinormal modes of black holes in f(T) gravity

Quasinormal modes of black holes in f(T) gravity

f(T, B) gravity with statistically fitting of H(z)

Quasinormal Modes of a Charged Black Hole with Scalar Hair

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