Quantum tunneling from rotating black holes with scalar hair in three dimensions

Сакалли, Иззет; Gürsel, Huriye

doi:10.1140/epjc/s10052-016-4158-x

Cited by 21 publications

(15 citation statements)

References 43 publications

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“…Moreover, spectroscopy of the black hole has been shows that the circumference of the charged hairy black hole is discrete and depends on the black hole parameters [6]. Therefore, mentioned 3D hairy black hole [7,8] was interesting subject of several issues due to relation with BTZ black hole and application in AdS/CFT correspondence. Here we would like to solve Klein-Gordon equation in a charged rotating 3D black hole with a scalar charge.…”

Section: Introductionmentioning

confidence: 99%

The Klein–Gordon equation of a rotating charged hairy black hole in (2 + 1) dimensions

Pourhassan

2016

Mod. Phys. Lett. A

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In this paper, we consider the Klein-Gordon equation in a 3D charged rotating hairy black hole background to study behavior of a massive scalar field. In the general case we find periodic-like behavior for the scalar field which may be vanishes at the black hole horizon or far from the black hole horizon. For the special cases of non-rotating or near horizon approximation we find radial solution of Klein-Gordon equation in terms of hypergeometric and Kummer functions. Also for the case of uncharged black hole we find numerical solution of the Klein-Gordon equation as periodic function which may enhanced out of the black hole or vanish at horizon. We find allowed boundary conditions which yield to the identical bosons described by scalar field.

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Section: Introductionmentioning

confidence: 99%

The Klein–Gordon equation of a rotating charged hairy black hole in (2 + 1) dimensions

Pourhassan

2016

Mod. Phys. Lett. A

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“…However, when the lens is spinning the path lengths will differ -shorter for co-rotating and longer for counter-rotating rays -giving rise to the time delay effect. 2 We shall consider deviation parameters that appear in the lowest order of expansion in a cr of the function 2g tφ g tt , since for the metric (1), the next order appears only in ( a cr ) 3 , reduced further by smaller order multiplicative terms like (M/r ) << 1 valid in the weak field. In this approximation, the expansion up to third order in (M/r ) is:…”

Section: Johannsen Metric and Relative Time Delaymentioning

confidence: 99%

“…The status of the no-hair theorem in general relativity is still a subject of current research ever since Penrose conjectured it in 1969 (see, e.g., a recent work by Cuzinatto et al [1]). Specific examples of spinning spacetimes have also been studied in the literature testing the theorem (see, e.g., [2]). However, to our knowledge, no generic spinning spacetime has been considered for such studies until Johannsen [3] proposed a new spinning metric that departs from the Kerr black hole (BH) by an infinite number of dimensionless deviation parameters such that non-zero value of any a e-mail: izmailov.ramil@gmail.com of them would indicate violation of the no-hair theorem.…”

Section: Introductionmentioning

confidence: 99%

Relative time delay in a spinning black hole as a diagnostic for no-hair theorem

Izmailov¹,

Zhdanov²,

Bhadra

et al. 2019

Eur. Phys. J. C

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The spinning regular black hole (spin a) metric proposed by Johannsen shares the Kerr horizon but contains independent dimensionless parameters marking deviation from the Kerr metric. Non-zero value of any of the parameters would indicate violation of the no-hair theorem. We shall find the influence of these parameters on the relative time delay (not Shapiro time delay) treated here as a diagnostic for no-hair theorem using aligned, finite, thinlens approximation in realistic spinning astrophysical configurations. Precise measurement of this delay would then help us determine, from observational perspective, whether or not any of the parameters is really non-zero. We shall also point out that the aligned spinning lens is completely equivalent to a "static" lens with a fictitious lens geometry, which would enable us to re-express the relative time delay components in terms of the spin a. Numerical values are tabulated for three astrophysical lens systems. The advantage of the present treatment is that it can accommodate a variety of spinning lens systems that are likely to be detected in the near future.

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“…Nowadays, various methods have been proposed to calculate the temperature of a black hole known as Hawking temperature. On the other hand, the Hamilton-Jacobi approach is an important version of the tunnelling method of the quantum mechanical point-like particles from a black hole [4][5][6][7][8][9][10][11][12][13][14][15][16][17][18][19][20]. Adopting this approach, Hawking temperature of various black holes were recovered by quantum tunnelling method of the particles across their event horizons.…”

Section: Introductionmentioning

confidence: 99%

Quantum gravity effect on the Hawking radiation of spinning dilaton black hole

Geçim

Sucu

2019

Eur. Phys. J. C

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The quantum gravity correction to the Hawking temperature of the 2+1 dimensional spinning dilaton black hole is studied by using the Hamilton-Jacobi approach in the context of the Generalized Uncertainty Principle (GUP). It is observed that the modified Hawking temperature of the black hole depends on both black hole and the tunnelling particle properties. Moreover, it is observed that the mass and the angular momentum of the scalar particle have the same effect on the Hawking temperature of the black hole, while the mass and total angular momentum (orbital+spin) of Dirac particle have different effect. Furthermore, the mass and total angular momentum (orbital+spin) of vector boson particle have a similar effect that of Dirac particle. Also, thermodynamical stability and phase transition of the black hole are discussed for scalar, Dirac and vector boson in the context of GUP, respectively. And, it is observed that the scalar particle probes the black hole as stable whereas, as for Dirac and vector boson particles, it might undergoes secondtype phase transition to become stable while in the absence of the quantum gravity effect all of these particle probes the black hole as stable.

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Quantum tunneling from rotating black holes with scalar hair in three dimensions

Cited by 21 publications

References 43 publications

The Klein–Gordon equation of a rotating charged hairy black hole in (2 + 1) dimensions

The Klein–Gordon equation of a rotating charged hairy black hole in (2 + 1) dimensions

Relative time delay in a spinning black hole as a diagnostic for no-hair theorem

Quantum gravity effect on the Hawking radiation of spinning dilaton black hole

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