Gravitational radiation in<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mi>D</mml:mi></mml:math>-dimensional spacetimes

Cardoso, Vítor; Dias, Óscar J. C.; Lemos, José P. S.

doi:10.1103/physrevd.67.064026

Cited by 264 publications

(429 citation statements)

References 62 publications

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“…To see how this might occur consider, for example, a binary system of black holes, or indeed any other source capable of emitting gravitational waves in D dimensions (see [24] for some recent discussion of gravitational waves and binary systems in higher dimensional GR). If our theory of gravity happens to contain freely propagating tensor ghosts, the energy of our JHEP12 (2008)038 source will increase as it emits waves carrying negative energy.…”

Section: Jhep12(2008)038mentioning

confidence: 99%

The instability of vacua in Gauss-Bonnet gravity

Charmousis

Padilla

2008

J. High Energy Phys.

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Owing to the quadratic nature of the theory, Einstein-Gauss-Bonnet gravity generically permits two distinct vacuum solutions. One solution (the "Einstein" vacuum) has a well defined limit as the Gauss-Bonnet coupling goes to zero, whereas the other solution (the "stringy" vacuum) does not. There has been some debate regarding the stability of these vacua, most recently from Deser & Tekin who have argued that the corresponding black hole solutions have positive mass and as such both vacua are stable. Whilst the statement about the mass is correct, we argue that the stringy vacuum is still perturbatively unstable. Simply put, the stringy vacuum suffers from a ghost-like instability that is not excited by the spherically symmetric black hole, but would be excited by any source likely to emit gravitational waves, such as a binary system. This result is reliable except in the strongly coupled regime close to the Chern-Simons limit, when the two vacua are almost degenerate. In this regime, we study instanton transitions between branches via bubble nucleation, and calculate the nucleation probability. This demonstrates that there is large mixing between the vacua, so that neither of them can accurately describe the true quantum vacuum. We also present a new gravitational instanton describing black hole pair production in de Sitter space on the Einstein branch, which is preferred to the usual Nariai instantons and is not present in pure Einstein gravity.

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Section: Jhep12(2008)038mentioning

confidence: 99%

The instability of vacua in Gauss-Bonnet gravity

Charmousis

Padilla

2008

J. High Energy Phys.

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“…The coefficients α are the coefficients of the expansioñ 26) are defined in the flat (n + 1)-dimensional Euclidean space. From .27) it follows .28) Multiplying by ω ′n , summing over p and integrating in dΩ (k) n dω ′ , we obtain .29) Finally, the normalization factor is…”

Section: Vector Perturbationsmentioning

confidence: 99%

“…The effective potential for tensor perturbations is equal to the potential of a massless scalar field in the higher-dimensional Schwarzschild black hole background [26].…”

Section: B Metric and Master Equations For Gravitational Perturbationsmentioning

confidence: 99%

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

Cardoso

Cavaglià

Gualtieri

2006

J. High Energy Phys.

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130

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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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“…Apart from [11], where gravitational bremsstrahlung of soft photons was studied in the context of string theory, the existing estimates of gravitational radiation either refer to phase (ii), or are based on the assumption of an already existing BH (e.g. radiation from particles falling into the BH [12]), on results of linearized theory relevant only to the case of non-gravitational scattering [8], on weakly relativistic numerical simulations [13] or again on collisions of waves in 4D [14]. For a related discussion see also [15].…”

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Transplanckian bremsstrahlung and black hole production

et al. 2010

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Classical gravitational bremsstrahlung in particle collisions at transplanckian energies is studied in M4 ×T d . The radiation efficiency ǫ ≡ E rad /E initial is computed in terms of the Schwarzschild radius rS( √ s), the impact parameter b and the Lorentz factor γcm and found to be ǫ = C d (rS/b) 3d+3 γ 2d+1 cm , larger than previous estimates by many powers of γcm ≫ 1. This means that in the ultrarelativistic case radiation loss becomes significant for b ≫ rS, so radiation damping must be taken into account in estimates of black hole production at transplanckian energies. The result is reliable for impact parameters in the overlap of γ ν rS < b < bc, ν = 1/2(d + 1), and b > λC , with bc marking (for d = 0) the loss of the notion of classical trajectories and λC ≡ /mc the Compton length of the scattered particles.Black hole (BH) production in LHC, predicted [1] in models with TeV-scale gravity and large extra dimensions [2-4] about ten years ago, has been the subject of intense theoretical study and numerical simulations (for a review see [5]). The prediction is based on the assumption that for impact parameters of the order of the horizon radius corresponding to the CM collision energy 2E = √ s(1) an event horizon should form due to the non-linear nature of gravity. Thewhere R is the large compactification radius. This classical, essentially, picture of BH formation is justified for transplanckian energies Indeed [6], in this case the D-dimensional Planck length l * = G D /c 3 1/(d+2) = /M * c and the de Broglie length of the collision λ B = c/ √ s satisfy the classicality condition λ B ≪ l * ≪ r S . Furthermore, gravity is believed to be the dominant force in the transplanckian region. Thus, for BH masses large compared to M * , the use of classical Einstein theory is well justified. Moreover, it seems that formation of BHs in four dimensions is predicted by string theory [7]. Thus, in spite of the fact that there are issues which require further study [8], a consensus has been reached that the prediction of BHs in ultra-high energy collisions is robust and is summarized in the widely accepted four-stage process of formation and evaporation of BHs in colliders [1,9], namely (i) formation of a closed trapped surface (CTS) in the collision of shock waves modeling the head-on particle collision, (ii) the balding phase, during which the BH emits gravitational waves and relaxes to the Myers-Perry BH, (iii) Hawking evaporation and superradiance phase in *

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Gravitational radiation inD-dimensional spacetimes

Cited by 264 publications

References 62 publications

The instability of vacua in Gauss-Bonnet gravity

The instability of vacua in Gauss-Bonnet gravity

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

Transplanckian bremsstrahlung and black hole production

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