Hawking radiation spectra for scalar fields by a higher-dimensional Schwarzschild–de Sitter black hole

Παππάς, Θωμάς; Kanti, Panagiota; Παππάς, Νικόλαος

doi:10.1103/physrevd.94.024035

Cited by 55 publications

(91 citation statements)

References 77 publications

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“…We will compare the numerical results with the approximate analytical ones and analysis the deviations stemming from various parameters. Our study is similar to the case of SdS black holes in [20].…”

Section: Introductionsupporting

confidence: 82%

“…Wheñ α is large, ξ decreases the effective potential and enhances the greybody factor. This is different from the Schwarzschild-de Sitter black hole where ξ always suppresses the greybody factor [20]. Figure 4: Effect of ξ on the greybody factor for different l. Solid lines for ξ = 0, dashed lines for ξ = 0.6.…”

Section: Competition Between ξ Andαmentioning

confidence: 89%

“…Without the GB term in the theory, the dependence of the greybody factors on the various parameters has been studied numerically in [20]. The results can be summarized as follows.…”

Section: Greybody Factor 41 Comparison Of Numerical and Analytical Rmentioning

confidence: 99%

“…It was shown furthermore that Hawking radiation is related to quasinormal modes and superradiance [15][16][17][18]. For more recent works, one can see [19][20][21][22][23][24][25][26][27][28][29].…”

Section: Introductionmentioning

confidence: 99%

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Hawking radiation for scalar fields by Einstein-Gauss-Bonnet–de Sitter black holes

Zhang

2019

Phys. Rev. D

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We study the greybody factor and power spectra of Hawking radiation for the minimally or nonminimally coupled scalar field with exact numerical method in spherically symmetric Einstein-Gauss-Bonnet-de Sitter black hole spacetime. The effects of scalar coupling constant, angular momentum number of scalar, spacetime dimension, cosmological constant and Gauss-Bonnet coupling constant on the Hawking radiation are studied in detail. Specifically, the Gauss-Bonnet coupling constant always increases the greybody factor in the entire energy regime.Different from the case of Schwarzschild-de Sitter black hole, the effects of the scalar coupling constant on the greybody factor are not monotonic but relevant to the values of Gauss-Bonnet coupling constant. Moreover, both these two coupling constants always suppress the power spectra of Hawking radiation in the whole energy regime. *

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Section: Introductionsupporting

confidence: 82%

Section: Competition Between ξ Andαmentioning

confidence: 89%

“…Without the GB term in the theory, the dependence of the greybody factors on the various parameters has been studied numerically in [20]. The results can be summarized as follows.…”

Section: Greybody Factor 41 Comparison Of Numerical and Analytical Rmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Hawking radiation for scalar fields by Einstein-Gauss-Bonnet–de Sitter black holes

Zhang

2019

Phys. Rev. D

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“…It would be interesting to investigate black hole evaporation process in de Sitter space-time (see, e.g. [44,45]). Furthermore, we apply the geometrical optics approximation and assume the emitted massless quanta move along null geodesics.…”

Section: Summary and Discussionmentioning

confidence: 99%

Black hole evaporation in Lovelock gravity with diverse dimensions

Yung

2019

Physics Letters B

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We investigate the black hole evaporation process in Lovelock gravity with diverse dimensions. By selecting the appropriate coefficients, the space-time solutions can possess a unique AdS vacuum with a fixed cosmological constant Λ = − (d−1)(d−2) 2ℓ 2 . The black hole solutions can be divided into two cases: d > 2k + 1 and d = 2k + 1. In the case of d > 2k + 1, the black hole is in an analogy with the Schwarzschild AdS black hole, and the life time is bounded by a time of the order of ℓ d−2k+1 , which reduces Page's result on the Einstein gravity in k = 1. In the case of d = 2k + 1, the black hole resembles the three dimensional black hole. The black hole vacuum corresponds to T = 0, so the black hole will take infinite time to evaporate away for any initial states, which obeys the third law of thermodynamics. In the asymptotically flat limit ℓ → ∞, the system reduces to the pure Lovelock gravity that only possesses the highest k-th order term. For an initial mass M0, the life time of the black hole is in the order of M d−2k+1 d−2k−1 0 .

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Regular Charged Black Holes, Energy Conditions, and Quasinormal Modes

Balart,

Panotopoulos,

Rincón

2023

Fortschritte der Physik

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Energy conditions and quasinormal modes (QNMs) for scalar perturbations of regular charged black holes within the framework of General Relativity coupled to non‐linear electrodynamics (NLE) are discussed. The frequencies are computed numerically adopting the WKB method, while in the eikonal limit an analytic expression for the spectra is obtained. The impact of the electric charge, the angular degree, and the overtone number on the spectra is investigated in detail. All frequencies are characterized by a negative imaginary part, and that each type of energy conditions imply a different quasinormal spectrum are found.

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Hawking radiation spectra for scalar fields by a higher-dimensional Schwarzschild–de Sitter black hole

Cited by 55 publications

References 77 publications

Hawking radiation for scalar fields by Einstein-Gauss-Bonnet–de Sitter black holes

Hawking radiation for scalar fields by Einstein-Gauss-Bonnet–de Sitter black holes

Black hole evaporation in Lovelock gravity with diverse dimensions

Regular Charged Black Holes, Energy Conditions, and Quasinormal Modes

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