Hawking radiation of Dirac fields in the (2+1)-dimensional black hole space-time

Hyun, Seungjoon; Song, Yong Seon; Yee, Jae Hyung

doi:10.1103/physrevd.51.1787

Cited by 9 publications

(7 citation statements)

References 10 publications

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“…The BTZ black hole is locally anti-de Sitter space, with global identifications. It will be interesting to see whether the solutions obtained here can be related to those obtained for AdS 3 in [16], modulo the global identifications.…”

Section: Equation Of Motion Of the Fermion In Btz Backgroundmentioning

confidence: 77%

Emission of fermions from BTZ black holes

Dasgupta

1999

Physics Letters B

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Section: Equation Of Motion Of the Fermion In Btz Backgroundmentioning

confidence: 77%

Emission of fermions from BTZ black holes

Dasgupta

1999

Physics Letters B

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“…The quantum field theory of a massless fermion in a static BTZ black hole background has been studied as well [51]. Hyun, Song, and Lee compute the two-point function for Dirichlet and Neumann boundary conditions at spatial infinity, again using the method of images (5.1), and study the response of a particle detector.…”

Section: Interiorsmentioning

confidence: 99%

The (2+1)-dimensional black hole

Carlip¹

1998

Quantum Gravity in 2+1 Dimensions

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I review the classical and quantum properties of the (2+1)dimensional black hole of Bañados, Teitelboim, and Zanelli. This solution of the Einstein field equations in three spacetime dimensions shares many of the characteristics of the Kerr black hole: it has an event horizon, an inner horizon, and an ergosphere; it occurs as an endpoint of gravitational collapse; it exhibits mass inflation; and it has a nonvanishing Hawking temperature and interesting thermodynamic properties. At the same time, its structure is simple enough to allow a number of exact computations, particularly in the quantum realm, that are impractical in 3+1 dimensions. * Since the seminal work of Deser, Jackiw, and 't Hooft [1,2,3] and Witten [4,5], general relativity in three spacetime dimensions has become an increasingly popular model in which to explore the foundations of classical and quantum gravity [6]. But although (2+1)-dimensional gravity has been widely recognized as a useful laboratory for studying conceptual issues-the nature of observables, for example, and the "problem of time"-it has been widely believed that the model is too physically unrealistic to give much insight into real gravitating systems in 3+1 dimensions. In particular, general relativity in 2+1 dimensions has no Newtonian limit [7] and no propagating degrees of freedom.It therefore came as a considerable surprise when Bañados, Teitelboim, and Zanelli (BTZ) showed in 1992 that (2+1)-dimensional gravity has a black hole solution [8]. The BTZ black hole differs from the Schwarzschild and Kerr solutions in some important respects: it is asymptotically anti-de Sitter rather than asymptotically flat, and has no curvature singularity at the origin. Nonetheless, it is clearly a black hole: it has an event horizon and (in the rotating case) an inner horizon, it appears as the final state of collapsing matter, and it has thermodynamic properties much like those of a (3+1)-dimensional black hole.The purpose of this article is to briefly review the past three years' work on the BTZ black hole. The first four sections deal with classical properties, while the last four discuss quantum mechanics, thermodynamics, and possible generalizations. For the most part, I will skip complicated derivations, referring the reader instead to the literature. For a recent review with a somewhat complementary choice of topics, see Ref. 9.The structure of the paper is as follows. In section 1, I introduce the BTZ solution in standard Schwarzschild-like coordinates and in Eddington-Finkelstein and Kruskal coordinates, and summarize its basic physical characteristics. Section 2 deals with the global geometry of the (2+1)-dimensional black hole, and outlines its description in the Chern-Simons formulation of (2+1)-dimensional general relativity. Section 3 describes the formation of BTZ black holes from collapsing matter, and reports on some recent work on critical phenomena, while section 4 summarizes the physics of black hole interiors, focusing on the phenomenon of mass inflation. I next turn to ...

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“…A neccessary condition for the viability of any quantum theory of AdS 3 gravity is the requirement that the semiclassical properties of the 3-dimensional BTZ-black holes [5] are correctly encoded in the microscopic theory. While the semi-classical Hawking radiation [6] is successfully reproduced in this formulation [7,8], Liouville theory fails to reproduce the entropy of the 3-dimensional BTZblack holes [9]. This inconsistency can be removed by embedding AdS 3 -gravity into super string theory on AdS 3 × S 3 × M 4 [10] which is dual to Q 5 D5 -and Q 1 D1 brane system on M 4 × S 1 .…”

Section: Introductionmentioning

confidence: 99%

Quasi-normal modes in topologically massive gravity

Sachs¹,

Solodukhin

2008

J. High Energy Phys.

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We determine the black hole quasi-normal mode spectrum for tensor perturbations in topologically massive AdS-gravity. In the special case of chiral gravity quasi-normal modes are absent despite of the presence of a horizon. In the process we uncover a simple algebraic structure in the quasi normal modes spectrum: the tower of QNM's consists of descendents of a "chiral highest weight" QNM which in turn satisfies a first order equation.

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Hawking radiation of Dirac fields in the (2+1)-dimensional black hole space-time

Cited by 9 publications

References 10 publications

Emission of fermions from BTZ black holes

Emission of fermions from BTZ black holes

The (2+1)-dimensional black hole

Quasi-normal modes in topologically massive gravity

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