Nonspherically Symmetric Collapse in Asymptotically AdS Spacetimes

Bantilan, H.; Figueras, Pau; Kunesch, Markus; Romatschke, Paul

doi:10.1103/physrevlett.119.191103

Cited by 24 publications

(44 citation statements)

References 44 publications

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“…In addition to the MyersPerry (and Kerr) family of rotating black holes, there are "black resonators" [65] which can be described as black holes with gravitational hair, and "geons" [10,35,61] which are horizonless gravitational configurations held together by their own self-gravity. The nonlinear dynamics of these solutions remain largely unexplored.Due to the lack of symmetries, the inclusion of angular momenta poses a numerical challenge (though see [66] for recent progress away from spherical symmetry). For instance, the dynamical problem for pure gravity in four dimensions requires a full 3+1 simulation.…”

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confidence: 99%

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Collapse and Nonlinear Instability of AdS Space with Angular Momentum

et al. 2017

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We present a numerical study of rotational dynamics in AdS5 with equal angular momenta in the presence of a complex doublet scalar field. We determine that the endpoint of gravitational collapse is a Myers-Perry black hole for high energies and a hairy black hole for low energies. We investigate the timescale for collapse at low energies E, keeping the angular momenta J ∝ E in AdS length units. We find that the inclusion of angular momenta delays the collapse time, but retains a t ∼ 1/E scaling. We perturb and evolve rotating boson stars, and find that boson stars near AdS appear stable, but those sufficiently far from AdS are unstable. We find that the dynamics of the boson star instability depend on the perturbation, resulting either in collapse to a Myers-Perry black hole, or development towards a stable oscillating solution.Introduction -Spacetimes with anti-de Sitter (AdS) boundary conditions play a central role in our understanding of gauge/gravity duality [1][2][3][4], where solutions to the Einstein equation with a negative cosmological constant are dual to states of strongly coupled field theories. This correspondence has inspired the study of gravitational physics in AdS over the past two decades.It is perhaps surprising that the issue of the nonlinear stability of (global) AdS was only raised nine years after AdS/CFT was first formulated [5,6]. Dafermos and Holzegel conjectured a nonlinear instability where the reflecting boundary of AdS allows for small but finite energy perturbations to grow and eventually collapse into a black hole. This is in stark contrast with Minkowksi and de Sitter spacetimes, where nonlinear stability has long been established [7,8].The first numerical evidence in favour of such an instability of AdS was reported in [9]. This topic has since attracted much attention both from numerical and formal perspectives . Remarkably, this instability has recently been proved for the spherically symmetric and pressureless Einstein-massless Vlasov system [62,63].The collapse timescale is dual to the thermalisation time in the field theory, and is important for characterising and understanding this instability. For energies E much smaller than the AdS length L = 1, early evolution is well-described by perturbation theory. However, irremovable resonances generically cause secular terms to grow, leading to a breakdown of perturbation theory at a time t ∼ 1/E. Numerical evidence suggests that horizon formation occurs shortly thereafter, i.e. at this same timescale. It is not fully understood why collapse seems to occur at the shortest timescale allowed by perturbation theory, though see [52] for some recent progress.However, all numerical studies have been restricted to zero angular momentum. Though perturbation theory breaks down at t ∼ 1/E for systems with rotation as well [10,53,64], this only places a lower bound on the timescale for gravitational collapse. It therefore remains unclear whether rotational forces could balance the gravitational attraction and delay the collapse time.The inc...

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confidence: 99%

“…Due to the lack of symmetries, the inclusion of angular momenta poses a numerical challenge (though see [66] for recent progress away from spherical symmetry). For instance, the dynamical problem for pure gravity in four dimensions requires a full 3+1 simulation.…”

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confidence: 99%

Collapse and Nonlinear Instability of AdS Space with Angular Momentum

et al. 2017

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“…Indeed, the closed walls are its necessary attribute. They are nucleated having the shape far from the spherical one [35,36,65,66]. The wall inhomogeneities are damped transferring the energy to the surrounding media and heating it.…”

Section: Resultsmentioning

confidence: 99%

“…The larger perturbations of wall surface survive by the moment t h of the horizon crossing. The nonspherical collapse with the BHs in final stage has been discussed in [65,66].…”

Section: Distribution Of Regions Over the Massmentioning

confidence: 99%

Clusters of Primordial Black Holes

et al. 2019

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The Primordial Black Holes (PBHs) are a well-established probe for new physics in the very early Universe. We discuss here the possibility of PBH agglomeration into clusters that may have several prominent observable features. The clusters can form due to closed domain walls appearance in the natural and hybrid inflation models whose subsequent evolution leads to PBH formation. The dynamical evolution of such clusters discussed here is of crucial importance. Such a model inherits all the advantages of uniformly distributed PBHs, like possible explanation of supermassive black holes existence (origin of the early quasars), the binary black hole mergers registered by LIGO/Virgo through gravitational waves, which could provide ways to test the model in future, the contribution to reionization of the Universe. If PBHs form clusters, they could alleviate or completely avoid existing constraints on the abundance of uniformly distributed PBHs, thus allowing PBH to be a viable dark matter candidate. Most of the existing constraints on uniform PBH density should be re-considered to the case of PBH clustering. Furthermore, unidentified cosmic gamma-ray point-like sources could be (partially) accounted. We conclude that models leading to PBH clustering are favored compared to models predicting the uniform distribution of PBHs.

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“…According to (39), (40) and (41), the expansion coefficients of the mass in terms of the parameterε areM…”

Section: Valuesmentioning

confidence: 99%

Anti–de Sitter geon families

Fodor

Forgács

2017

Phys. Rev. D

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A detailed perturbative construction of globally regular, asymptotically anti-de Sitter (AdS) time-periodic solutions of Einstein's equations with a negative cosmological constant (AdS geons) is presented. Starting with the most general superposition of the l = 2 even parity (scalar) eigenmodes of AdS at linear order, it is shown that at the fifth order in perturbation theory one obtains five one-parameter geon families, two of which have a helical Killing vector, one with axial symmetry, and two others without continuous symmetries. The details and some subtle aspects of the perturbative expansions are also presented.

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Nonspherically Symmetric Collapse in Asymptotically AdS Spacetimes

Cited by 24 publications

References 44 publications

Collapse and Nonlinear Instability of AdS Space with Angular Momentum

Collapse and Nonlinear Instability of AdS Space with Angular Momentum

Clusters of Primordial Black Holes

Anti–de Sitter geon families

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