Black hole evaporation and large extra dimensions

Casadio, Roberto; Harms, B.

doi:10.1016/s0370-2693(00)00840-6

Cited by 77 publications

(75 citation statements)

References 22 publications

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“…Other related research included a relation between the GL transition and gauge theories through Matrix M-Theory [19], a prediction for a non-uniform near-extremal black string [20], a useful review of numerical relativity [21], a relation between the GL instability and the negative heat capacity of black holes [22], a discussion of implication of the GL instability to more general spacetimes with horizons [23], a discussion of the explosion expected during these phase transition [24], a recent analysis of 4d metrics with a compact dimension but different asymptotic conditions and a study of non-uniform strings in the two-brane system [26]. See also [27,28,29] for a short and non-representative list of papers on black holes and large extra dimensions/ brane worlds/ accelerator prospects.…”

Section: Introductionmentioning

confidence: 99%

Caged black holes: Black holes in compactified spacetimes. I. Theory

2004

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In backgrounds with compact dimensions there may exist several phases of black objects including the black-hole and the black-string. The phase transition between them raises puzzles and touches fundamental issues such as topology change, uniqueness and Cosmic Censorship. No analytic solution is known for the black hole, and moreover, one can expect approximate solutions only for very small black holes, while the phase transition physics happens when the black hole is large. Hence we turn to numerical solutions. Here some theoretical background to the numerical analysis is given, while the results will appear in a forthcoming paper. Goals for a numerical analysis are set. The scalar charge and tension along the compact dimension are defined and used as improved order parameters which put both the black hole and the black string at finite values on the phase diagram. Predictions for small black holes are presented. The differential and the integrated forms of the first law are derived, and the latter (Smarr's formula) can be used to estimate the "overall numerical error". Field asymptotics and expressions for physical quantities in terms of the numerical ones are supplied. Techniques include "method of equivalent charges", free energy, dimensional reduction, and analytic perturbation for small black holes.

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Section: Introductionmentioning

confidence: 99%

Caged black holes: Black holes in compactified spacetimes. I. Theory

2004

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“…In this case the horizon pinches off and the central singularity becomes "naked". By now there is a rapidly growing amount of the literature on the subject [3][4][5][6][7][8][9][10][11][12][13][14][15][16][17][18][19][20][21]. In particular the scenario of GL was questioned by Horowitz and Maeda (HM) [3] who, on grounds of the classical "no tear" property of the horizons, argued that horizon pinching is impossible and hence a decaying string settles to another stable phase -a non-uniform black string(NUBS).…”

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confidence: 99%

Critical Dimension in the Black-String Phase Transition

2004

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In spacetimes with compact dimensions there exist several black object solutions including the black-hole and the black-string. These solutions may become unstable depending on their relative size and the relevant length scale set by the compact dimensions. The transition between these solutions raises puzzles and addresses fundamental questions such as topology change, uniquenesses and cosmic censorship. Here, we consider black strings wrapped over the compact circle of a d-dimensional cylindrical spacetime. We construct static perturbative non-uniform string solutions around the instability point of a uniform string. First we compute the instability mass for a large range of dimensions, d, and find that it follows essentially an exponential law γ d , where γ is a constant. Then we determine that there is a critical dimension, d * = 13, such that for d ≤ d * the phase transition between the uniform and the non-uniform strings is of first order, while for d > d * , it is, surprisingly, of higher order.

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“…In our Monte Carlo simulation, we model the black hole decay as the sequential emission of individual partons [15]. We derive the ω and angular momentum ( j) spectra using the micro-canonical ensemble [16] …”

Section: Black Hole Decaymentioning

confidence: 99%

Production and decay of spinning black holes at colliders and tests of black hole dynamics

Kotwal

Hays

2002

Phys. Rev. D

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We analyse the angular momentum distribution of black holes produced in high energy collisions in space-times with extra spatial dimensions. We show that the black hole spin significantly affects the energy and angular spectra of Hawking radiation. Our results show the experimental sensitivity to the angular momentum distribution and provide tests of black hole production dynamics.Typeset using REVT E X 1

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Black hole evaporation and large extra dimensions

Cited by 77 publications

References 22 publications

Caged black holes: Black holes in compactified spacetimes. I. Theory

Caged black holes: Black holes in compactified spacetimes. I. Theory

Critical Dimension in the Black-String Phase Transition

Production and decay of spinning black holes at colliders and tests of black hole dynamics

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