Gravitational signatures of a non-commutative stable black hole

Heidari, N.; Hassanabadi, H.; Araújo Filho, A.A.; Kr̆íz̆, J.; Zare, S.; Porfírio, P.J.

doi:10.1016/j.dark.2023.101382

Cited by 7 publications

(3 citation statements)

References 119 publications

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“…where K is commonly referred to as the Carter constant [90,91]. Following a series of algebraic manipulations, the resulting expression is: In our quest to determine the radius of the shadow, we will employ the celestial coordinates α and β [73,[92][93][94] as: α = −ξ and β = ± √ η. Thereby, we are able to write the radius shadow as follows…”

Section: Photon Sphere and Shadowsmentioning

confidence: 99%

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Exploring antisymmetric tensor effects on black hole shadows and quasinormal frequencies

Araújo Filho,

Reis,

Hassanabadi

2024

J. Cosmol. Astropart. Phys.

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This study explores the impact of antisymmetric tensor effects on spherically symmetric black holes, investigating photon spheres, shadows, emission rate and quasinormal frequencies in relation to a parameter which triggers the Lorentz symmetry breaking. We examine these configurations without and with the presence of a cosmological constant. In the first scenario, the Lorentz violation parameter, denoted as λ, plays a pivotal role in reducing both the photon sphere and the shadow radius, while also leading to a damping effect on quasinormal frequencies. Conversely, in the second scenario, as the values of the cosmological constant (Λ) increase, we observe an expansion in the shadow radius. Also, we provide the constraints of the shadows based on the analysis observational data obtained from the Event Horizon Telescope (EHT) focusing on Sagittarius A* shadow images. Additionally, with the increasing Λ, the associated gravitational wave frequencies exhibit reduced damping modes.

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Section: Photon Sphere and Shadowsmentioning

confidence: 99%

“…Recent literature has seen similar examinations of quasinormal modes within various frameworks, including non-commutativity [94,112], bumblebee gravity [73], regular black holes [71,84], and more. For the computation of these quasinormal modes, our methodology centers on the WKB approach.…”

Section: Jcap05(2024)029mentioning

confidence: 99%

Exploring antisymmetric tensor effects on black hole shadows and quasinormal frequencies

Araújo Filho,

Reis,

Hassanabadi

2024

J. Cosmol. Astropart. Phys.

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“…Basically, BHs can be interpreted as the thermal systems that have an associated temperature and entropy; therefore, BHs produce radiation, and such radiation is called Hawking radiation [63]. In the literature, the WKB method has been used to obtain reflection and transmission coefficients (greybody factors) [64][65][66][67][68], such as in the context of braneworld models and wormholes. In this section, we intend to discuss the frequency-dependent reflection R(ω) and transmission coefficient T(ω) for a scattering process of the gravitational and electromagnetic perturbations from the Bardeen-Kiselev BH with the cosmological constant.…”

Section: Greybody Factors and Absorption Coefficientsmentioning

confidence: 99%

Probing the Bardeen–Kiselev black hole with the cosmological constant caused by Einstein equations coupled with nonlinear electrodynamics using quasinormal modes and greybody bounds

Wu,

Wang,

Long

2024

Commun. Theor. Phys.

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In this work, we investigate a static and spherically symmetric Bardeen–Kiselev black hole (BH) with the cosmological constant, which is a solution of the Einstein-non-linear Maxwell field equations. We compute the quasinormal frequencies for the Bardeen–Kiselev BH with the cosmological constant due to electromagnetic and gravitational perturbations. By varying the BH parameters, we discuss the behavior of both real and imaginary parts of the BH quasinormal frequencies and compare these frequencies with the Reissner–Nordström–de Sitter BH surrounded by quintessence (RN-dSQ). Interestingly, it is shown that the responses of the Bardeen–Kiselev BH with the cosmological constant and the RN-dSQ under electromagnetic perturbations are different when the charge parameter q, the state parameter w and the normalization factor c are varied; however, for the gravitational perturbations, the responses of the Bardeen–Kiselev BH with the cosmological constant and the RN-dSQ are different only when the charge parameter q is varied. Therefore, compared with the gravitational perturbations, the electromagnetic perturbations can be used to understand nonlinear and linear electromagnetic fields in curved spacetime separately. Another interesting observation is that, due to the presence of Kiselev quintessence, the electromagnetic perturbations around the Bardeen–Kiselev BH with the cosmological constant damps faster and oscillates slowly; for the gravitational perturbations, the quasinormal mode decays slowly and oscillates slowly. We also study the reflection and transmission coefficients along with the absorption cross section in the Bardeen–Kiselev BH with the cosmological constant; it is shown that the transmission coefficients will increase due to the presence of Kiselev quintessence.

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