Quantum tunneling and quasinormal modes in the spacetime of the Alcubierre warp drive

Jusufi, Kimet; Сакалли, Иззет; Овгун, Али

doi:10.1007/s10714-017-2330-8

Cited by 23 publications

(4 citation statements)

References 151 publications

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“…To calculate the weak deflection angle, Gibbons & Werner (2008) proposed a new method by using the Gauss-Bonnet theorem. Gibbons & Werner's method has been applied to the BH as well as to the wormhole (Werner 2012;Jusufi 2017;Crisnejo & Gallo 2018;Jusufi et al 2019;Ovgun et al 2019;Li & Ovgun 2020;Li & Zhou 2020) in the literature. Here, we apply this method to calculate the weak deflection angle by acoustic charged BH for the cases where the receiver and source are located at an infinite distance from the BH (lens).…”

Section: Weak Gravitational Lensing By Acoustic Charged Bhmentioning

confidence: 99%

Gravitational Lensing of Acoustic Charged Black Holes

Molla

Debnath

2023

ApJ

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We study the gravitational lensing of acoustic charged black holes in strong and weak field limit approximations. For this purpose, we first numerically obtain the deflection limit coefficients and deflection angle in the strong field limit. We observe that the strong deflection angle α D increases with increasing magnitude of the charged parameter Q and that the strong deflection angle α D of an acoustic charged black hole with tuning parameter ξ = 4 is greater than that of a standard Reissner–Nordström black hole (ξ = 0). We also study the astrophysical consequences via strong gravitational lensing by taking the example of various supermassive black holes in the center of several galaxies and observe that the acoustic charged black hole could be quantitatively distinguished from standard Reissner–Nordström (ξ = 0) and standard Schwarzschild (ξ = 0, Q = 0) black holes. Furthermore, by using the Gauss–Bonnet theorem, we derive the weak deflection angle in the background of an acoustic charged black hole in the curved spacetime. We find that, for fixed values of the charged parameter Q and the tuning parameter (ξ = 0 or 4), the weak deflection angle σ D decreases with the impact parameter b. We also observe that the weak deflection angle σ D decreases with increasing magnitude of the charged parameter Q for a fixed value of the tuning parameter (ξ = 0 or 4). Our results suggest that the observational test for an acoustic charged black hole is indeed feasible, and it is generalized to the cases of acoustic Schwarzschild (Q = 0), standard Reissner–Nordström (ξ = 0), and standard Schwarzschild (ξ = 0, Q = 0) black holes.

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Section: Weak Gravitational Lensing By Acoustic Charged Bhmentioning

confidence: 99%

Gravitational Lensing of Acoustic Charged Black Holes

Molla

Debnath

2023

ApJ

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“…It is worth noting that in order the waves to be ingoing and outgoing as shown above, we impose a condition, which is named as the wave type identifier conditionby [89][90][91]]…”

Section: A Exact Solution Of the Radial Equation And Qnmsmentioning

confidence: 99%

Analytical solutions in a cosmic string Born–Infeld-dilaton black hole geometry: quasinormal modes and quantization

2018

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Chargeless massive scalar fields are studied in the spacetime of Born-Infeld dilaton black holes (BIDBHs). We first separate the massive covariant Klein-Gordon equation into radial and angular parts and obtain the exact solution of the radial equation in terms of the confluent Heun functions.Using the obtained radial solution, we show how one gets the exact quasinormal modes (QNMs) for some particular cases. We also solve the Klein-Gordon equation in the spacetime of BIDBH with a cosmic string in which we point out the effect of the conical deficit on the BIDBH. The analytical solutions of the radial and angular parts are obtained in terms of the confluent Heun functions. Finally, we study the quantization of the BIDBH. While doing this, we also discuss the Hawking radiation in terms of the effective temperature.

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“…After LIGO's great successes about the gravitational wave measurements [33], the subject of QNMs has gained considerable importance in the direct identification of BHs. Today, there are numerous well-known studies which show that the surrounding geometry of a BH experiences QNMs under perturbations (see for example [34][35][36][37][38][39][40][41] and references therein). One of the most important features to know about QNMs is that they allow us to analyze the quantum entropy/area spectrum of the BHs.…”

Section: Introductionmentioning

confidence: 99%