Black Holes Radiate Mainly on the Brane

Emparan, Roberto; Horowitz, Gary T.; Myers, Robert C.

doi:10.1103/physrevlett.85.499

Cited by 393 publications

(486 citation statements)

References 14 publications

(5 reference statements)

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“…From the bulk point of view, this effect is a classical one, which arises because a black hole stuck on a brane is accelerating through the AdS bulk. The classical emission of bulk radiation by these large black holes will overshadow the quantum radiation considered in [7]. The radiation we are considering only looks quantum once one turns to the dual CFT+gravity, where the largesse of this effect compared to the emission of brane modes is due to the huge number of CFT degrees of freedom -which is in turn the dual of the huge ratio (L/L P 4 ) 2 .…”

Section: Introductionmentioning

confidence: 99%

“…Still, one sees from it that the rate of Hawking evaporation diminishes significantly, as suggested by the classical bulk picture argument. A small black hole Hawking-radiates mostly along the brane, since the dominant s-wave channel cannot discriminate between the bulk and the localized gravity [7]. This evaporation is much slower than the emission of a large number of CFT modes.…”

Section: Introductionmentioning

confidence: 99%

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Black Hole Astrophysics in AdS Braneworlds

Emparan¹,

García-Bellido²,

Kaloper³

2003

J. High Energy Phys.

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100

102

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We consider astrophysics of large black holes localized on the brane in the infinite RandallSundrum model. Using their description in terms of a conformal field theory (CFT) coupled to gravity, deduced in Ref.[1], we show that they undergo a period of rapid decay via Hawking radiation of CFT modes. For example, a black hole of mass few × M ⊙ would shed most of its mass in ∼ 10 4 − 10 5 years if the AdS radius is L ∼ 10 −1 mm, currently the upper bound from table-top experiments. Since this is within the mass range of X-ray binary systems containing a black hole, the evaporation enhanced by the hidden sector CFT modes could cause the disappearance of X-ray sources on the sky. This would be a striking signature of RS2 with a large AdS radius. Alternatively, for shorter AdS radii, the evaporation would be slower. In such cases, the persistence of X-ray binaries with black holes already implies an upper bound on the AdS radius of L < ∼ 10 −2 mm, an order of magnitude better than the bounds from table-top experiments. The observation of primordial black holes with a mass in the MACHO range M ∼ 0.1 − 0.5 M ⊙ and an age comparable to the age of the universe would further strengthen the bound on the AdS radius to L < ∼ few × 10 −6 mm. 1 roberto.emparan@cern.ch 2

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Black Hole Astrophysics in AdS Braneworlds

Emparan¹,

García-Bellido²,

Kaloper³

2003

J. High Energy Phys.

Self Cite

100

102

View full text Add to dashboard Cite

show abstract

“…From the above equations it follows 6) i.e. the wave Ψ (λ,ω) describes one ingoing particle per unit time.…”

Section: Appendix: Derivation Of the Cross Sectionsmentioning

confidence: 99%

“…Moreover, brane emission should dominate over bulk emission because standard model fields carry a larger number of d.o.f. than the graviton [6]. However, a black hole does not radiate exactly as a black body and the emission spectrum depends crucially on the structure and dimensionality of the spacetime.…”

Section: Introductionmentioning

confidence: 99%

Hawking emission of gravitons in higher dimensions: non-rotating black holes

Cardoso

Cavaglià

Gualtieri

2006

J. High Energy Phys.

130

133

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We compute the absorption cross section and the total power carried by gravitons in the evaporation process of a higher-dimensional non-rotating black hole. These results are applied to a model of extra dimensions with standard model fields propagating on a brane. The emission of gravitons in the bulk is highly enhanced as the spacetime dimensionality increases. The implications for the detection of black holes in particle colliders and ultrahigh-energy cosmic ray air showers are briefly discussed.

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“…Introduction: An exciting consequence of TeV-scale quantum gravity [1] is the possibility of producing black holes (BHs) [2][3][4][5][6] at the LHC and beyond. Simple estimates of their production cross section, treating the BHs as general relativistic (GR) objects, suggest enormous event rates at the LHC -as large as a BH per sec [5,6].…”

mentioning

confidence: 99%

String balls at the LHC and beyond

2002

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In string theory, black holes have a minimum mass below which they transition into highly excited long and jagged strings -"string balls". These are the stringy progenitors of black holes; because they are lighter, in theories of TeV-gravity, they may be more accessible to the LHC or the VLHC. They share some of the characteristics of black holes, such as large production cross sections. Furthermore, they evaporate thermally at the Hagedorn temperature and give rise to high-multiplicity events containing hard primary photons and charged leptons, which have negligible standard-model background. * Also at Depto. de Física Teórica, Universidad del País Vasco, Bilbao, Spain 1 Introduction: An exciting consequence of TeV-scale quantum gravity [1] is the possibility of producing black holes (BHs) [2][3][4][5][6] at the LHC and beyond. Simple estimates of their production cross section, treating the BHs as general relativistic (GR) objects, suggest enormous event rates at the LHC -as large as a BH per sec [5,6]. Furthermore, decays of the BHs into hard primary photons or charged leptons are a clean signature for detection, with negligible standard model background. The production and decay of the experimentally most accessible light black holes -those with mass M BH near the fundamental Planck scale M P ∼ TeV-is clouded by string-theoretic uncertainties. The purpose of this paper is to discuss these and point out the possible presence and properties of light stringy progenitors of the black holes.According to string theory, the minimum mass M min above which a black hole can be treated general-relativistically is M min ∼ Ms

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Black Holes Radiate Mainly on the Brane

Cited by 393 publications

References 14 publications

Black Hole Astrophysics in AdS Braneworlds

Black Hole Astrophysics in AdS Braneworlds

Hawking emission of gravitons in higher dimensions: non-rotating black holes

String balls at the LHC and beyond

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