Remarks on the effects of the quintessence on regular black holes

Maluf, R. V.; Muniz, C. R.; Santos, A. C. L.

doi:10.1007/s10509-022-04118-6

Cited by 5 publications

(2 citation statements)

References 16 publications

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“…In conclusion, since the regular Kiselev BH solution family overcomes the singularity problem theoretically and the celestial model described by it is more in line with the actual situation, this kind of BH solution family has received considerable attention from scholars [24][25][26]. We are also very interested in this kind of BH spacetime.…”

Section: Introductionmentioning

confidence: 91%

“…In this section, our purpose is to discuss the QNMs and the stability of the perturbations in the Bardeen-Kiselev BH with athe cosmological constant spacetime, especially for the QNMs of the Bardeen-Kiselev BH with the cosmological constant for gravitational and electromagnetic perturbations. QNMs for a perturbed BH spacetime are the solutions to the wave equation given in equations ( 16) and (26), and to derive these solutions, it is necessary to impose proper boundary conditions: However, it is tricky to analytically solve the timeindependent second-order differential equation (such as equation ( 16)) with the potential (such as equation ( 15)) for a nonlinear magnetically charged BH with the cosmological constant surrounded by Kiselev quintessence. The WKB method can be used for the effective potential, which configurates the form of a potential barrier and takes constant values at the event horizon and spatial infinity.…”

Section: The Qnms Of the Bardeen-kiselev Bh With The Cosmological Con...mentioning

confidence: 99%

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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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Section: Introductionmentioning

confidence: 91%

Section: The Qnms Of the Bardeen-kiselev Bh With The Cosmological Con...mentioning

confidence: 99%