Black hole solutions in braneworlds with induced gravity

Kofinas, Georgios; Papantonopoulos, Eleftherios; Zamarias, Vassilios

doi:10.1103/physrevd.66.104028

Cited by 88 publications

(67 citation statements)

References 49 publications

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“…In this spirit, black hole and wormhole solutions [6,9,16,17] as well as star solutions on the brane [18] have been obtained in the last years. We should mention that even without relaxing this condition, previous solutions have also been found [19,20]. In this context the hamiltonian constraint can be written explicitly in terms of A and B as [6,9] B A ′′ A − 1 2…”

Section: Brane Black Hole Solutionsmentioning

confidence: 99%

Stability and thermodynamics of brane black holes

et al. 2006

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Section: Brane Black Hole Solutionsmentioning

confidence: 99%

Stability and thermodynamics of brane black holes

et al. 2006

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“…In addition, it suffers from a Gregory-Laflamme instability [60,61]. Despite the numerous attempts to derive a regular, asymptotically AdS blackhole solution localised on a brane with a non-vanishing tension (for an indicative list of papers, see [62,63,64,65,66,67,68,69,70,71,72]; for a more complete list of references, see [30,31,32]), up to today no analytical solution has been constructed. Numerical studies [73,74,75] found black-hole solutions with horizon radius smaller than or of the order of the AdS length ℓ AdS in the context of five-and six-dimensional warped models.…”

Section: Black Holes In Rs Brane-worldsmentioning

confidence: 99%

Hawking Radiation from Higher-Dimensional Black Holes

Kanti

Winstanley

2014

Fundamental Theories of Physics

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Summary. We review the quantum field theory description of Hawking radiation from evaporating black holes and summarize what is known about Hawking radiation from black holes in more than four space-time dimensions. In the context of the Large Extra Dimensions scenario, we present the theoretical formalism for all types of emitted fields and a selection of results on the radiation spectra. A detailed analysis of the Hawking fluxes in this case is essential for modelling the evaporation of higher-dimensional black holes at the LHC, whose creation is predicted by lowenergy models of quantum gravity. We discuss the status of the quest for black-hole solutions in the context of the Randall-Sundrum brane-world model and, in the absence of an exact metric, we review what is known about Hawking radiation from such black holes.

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“…Note that the solutions (21)- (25) are the generic braneworld solutions and have been obtained without any assumption for the bulk space. It is now obvious that the only possible static exterior solution (15), surrounding the collapsing region, cannot take one of the permissible forms (21), (22), (24) of induced-gravity theory, which means that the no-go theorem for induced gravity has been proved.…”

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confidence: 99%

“…For spherically symmetric braneworld metrics of the form (12), the system of Eqs. (16)- (20) was fully integrated in vacuum in [14], [15], and the results are as follows. For E µ ν = 0 on the brane, the solution is Schwarzschild-(A)dS 4…”

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Gravitational collapse in braneworld models with curvature corrections

Kofinas

Papantonopoulos

2004

J. Cosmol. Astropart. Phys.

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We study the collapse of a homogeneous braneworld dust cloud in the context of the various curvature correction scenarios, namely, the induced-gravity, the Gauss-Bonnet, and the combined induced-gravity and Gauss-Bonnet. In accordance to the Randall-Sundrum model, and contrary to four-dimensional general relativity, we show in all cases that the exterior spacetime on the brane is non-static.In this Letter, we discuss the Oppenheimer-Snyder-like collapse on a brane in the context of curvature correction terms. In the Randall-Sundrum scenario, this problem has been analyzed in [1], and found that, contrary to the general relativity case, the vacuum exterior of a spherical cloud is non-static. This is a result of modification of the effective Einstein equations on the brane with local and non-local terms representing high energy corrections to general relativity. The non-static nature of the exterior metric mainly arises because of the presence of bulk graviton stresses, which transmit effects non-locally from the interior to the exterior on the brane, and of the nonvanishing of the effective pressure at the boundary surface [2], which connects the interior with exterior metric via the four dimensional matching conditions.We derive here the same result within the inducedgravity, the Gauss-Bonnet, and the combined GaussBonnet and induced gravity braneworld models. In all these models, the effective Einstein equations on the brane are modified by local and non-local terms, which are much more complicated than the corresponding terms in the Randall-Sundrum case, but nevertheless, the nonstaticity arises because of a mismatch of the interior with the exterior metric on the boundary collapsing surface.We consider for convenience and without loss of generality the extra-dimensional coordinate y such that the brane is fixed at y = 0. The induced metric h µν on this hypersurface is defined by h AB = g AB − n A n B , with n A the unit vector normal to the brane (µ, ν = 0, 1, 2, 3; A, B = 0, 1, 2, 3, 5). The total action of the system is taken to bewhere R, R are the Ricci scalars of the metrics g AB and * kofinas@cecs.cl † lpapa@central.ntua.gr h AB respectively. The Gauss-Bonnet coupling α has dimensions (length) 2 and is defined aswith g s the string energy scale, while the induced-gravity crossover lenght scale r c isHere, the fundamental (M 5 ) and the four-dimensional (M 4 ) Planck masses are given byThe brane tension is given byand is non-negative. (Note that Λ 4 is not the same as the cosmological constant on the brane.)The collapse region has in comoving coordinates a Robertson-Walker metricwhere the scale factor a(τ ) is given by the modified Friedmann equation of the corresponding model, while the energy density is given by the usual dust law ρ = ρ 0 (a 0 /a) 3 , with a 0 standing for the epoch when the cloud started to collapse. This Friedmann equation can also be written in terms of the proper radius from the center of the cloud r(τ ) = a(τ )χ/(1+kχ 2 /4) of the collapsing boundary surface at χ = χ 0 .Concerning...

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Black hole solutions in braneworlds with induced gravity

Cited by 88 publications

References 49 publications

Stability and thermodynamics of brane black holes

Stability and thermodynamics of brane black holes

Hawking Radiation from Higher-Dimensional Black Holes

Gravitational collapse in braneworld models with curvature corrections

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