Stability and Thermodynamics of Brane Black Holes

Instituto de Física, Universidade de São Paulo, C.P. 66318, 05315-970 São Paulo, SP, Brazil
Journal of Physics Conference Series 05/2006; 752(1-2):40-59. DOI: 10.1016/j.nuclphysb.2006.06.017
Source: arXiv


We consider scalar and axial gravitational perturbations of black hole solutions in brane world scenarios. We show that perturbation dynamics is surprisingly similar to the Schwarzschild case with strong indications that the models are stable. Quasinormal modes and late-time tails are discussed. We also study the thermodynamics of these scenarios verifying the universality of Bekenstein's entropy bound as well as the applicability of 't Hooft's brickwall method. (c) 2006 Elsevier B.V. All rights reserved.

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Available from: E. Abdalla, Oct 07, 2015
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    • "Brane world models perform a distinct bough in high energy physics, owning plenty of ideas inspired on advances in string theory [1]. Precursory efforts deal with a brane world Universe [2] [3] [4], with cosmological and astrophysical implications comprehensively investigated in the literature [5] [6] [7] [8] [9] [10] [11] [12] [13] [14] [15] [16] [17] [18] [19] [20] [21], as well as 5D effects evinced from the gravitational collapse proposed in, e. g., [22–30, 32–36]. The Universe is well known to go through a phase of the accelerated expansion, supported by the recent observational data [37] [38], what could be accounted for either dark energy or modified theories of gravity [22, 39–41] as well. "
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    ABSTRACT: The perihelion precession, the deflection of light, and the radar echo delay are classical tests of General Relativity here used to probe brane world topologically charged black holes in a f(R) bulk and to constrain the parameter that arises from the Shiromizu-Maeda-Sasaki procedure applied to a f(R) bulk as well. The existing Solar system observational data constrain the possible values of the tidal charge parameter and the effective cosmological constant including f(R) brane world effects. We show that the observational/experimental data for both perihelion precession and radar echo delay make the black hole space of parameters to be more strict than the ones for the Dadhich, Maartens, Papadopoulos and Rezania (DMPR) black hole geometry. Furthermore, the deflection of light constrains the tidal charge parameter similarly as the DMPR black holes due to a peculiarity in the equation of motion.
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    • "For additional information about QNM's see the following reviews [10] [11]. Our previous experience on black hole perturbations in many different contexts can be seen in [12] [13] [14] [15]. "
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    ABSTRACT: In this work we describe an interesting application of a simple derivative-free optimization method to extract the quasinormal modes (QNM's) of a massive scalar field propagating in a 4-dimensional Schwarzschild anti-de Sitter black hole (Sch-AdS$_4$). In this approach, the problem to find the QNM's is reduced to minimize a real valued function of two variables and does not require any information about derivatives. In fact, our strategy requires only evaluations of the objective function to search global minimizers of the optimization problem. Firstly, numerical experiments were performed to find the QNM's of a massless scalar field propagating in intermediate and large Sch-AdS$_4$ black holes. The performance of this optimization algorithm was compared with other numerical methods used in previous works. Our results showed to be in good agreement with those obtained previously. Finally, the massive scalar field case and its QNM's were also obtained and discussed.
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    ABSTRACT: By introducing the generalized uncertainty principle, we calculate the entropy of the bulk scalar field on the Randall-Sundrum brane background without any cutoff. We obtain the entropy of the massive scalar field proportional to the horizon area. Here, we observe that the mass contribution to the entropy exists in contrast to all previous results, which is independent of the mass of the scalar field, of the usual black hole cases with the generalized uncertainty principle. Comment: 12 pages. The improved version published in Phys. Rev. D
    Physical review D: Particles and fields 05/2006; 74(10). DOI:10.1103/PhysRevD.74.104001 · 4.86 Impact Factor
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