Lifetime of unstable hairy black holes

Hod, Shahar

doi:10.1016/j.physletb.2008.02.010

Cited by 22 publications

(17 citation statements)

References 43 publications

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“…It is interesting to compare the eigenvalues of the Reissner-Nordström solution with a bound on the lifetime of unstable hairy black holes proposed by Hod [29], based on arguments from quantum information theory. This bound was shown in [29] to be satisfied for the n = 1 colored black hole but the situation for the Reissner-Nordström solution remained inconclusive. The bound implies that the eigenvalues should be bounded by…”

Section: Mode Analysismentioning

confidence: 99%

“…In the strong bound, ∆E is the mass that is swallowed by the unstable black hole in a nonlinear evolution. As a first approximation, this was taken in [29] to be the entire mass outside the horizon of the initial black hole, ∆E = ∆M max = M − 1 2 R h . For the Reissner-Nordström solution, we have Figure 2 shows that close to the extremal value R h = 1, only the weak bound is satisfied, whereas the above version of the strong bound is violated (unlike for the colored black holes, where both are satisfied [29]).…”

Section: Mode Analysismentioning

confidence: 99%

“…As a first approximation, this was taken in [29] to be the entire mass outside the horizon of the initial black hole, ∆E = ∆M max = M − 1 2 R h . For the Reissner-Nordström solution, we have Figure 2 shows that close to the extremal value R h = 1, only the weak bound is satisfied, whereas the above version of the strong bound is violated (unlike for the colored black holes, where both are satisfied [29]). However, ∆E should really be taken to be the actual amount of hair that falls into the black hole; this will be computed in the following section.…”

Section: Mode Analysismentioning

confidence: 99%

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Formation and decay of Einstein-Yang-Mills black holes

Rinne

2014

Phys. Rev. D

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We study various aspects of black holes and gravitational collapse in Einstein-Yang-Mills theory under the assumption of spherical symmetry. Numerical evolution on hyperboloidal surfaces extending to future null infinity is used. We begin by constructing colored and Reissner-Nordström black holes on surfaces of constant mean curvature and analyze their perturbations. These linearly perturbed black holes are then evolved into the nonlinear regime and the masses of the final Schwarzschild black holes are computed as a function of the initial horizon radius. We compare with an information-theoretic bound on the lifetime of unstable hairy black holes derived by Hod. Finally we study critical phenomena in gravitational collapse at the threshold between different Yang-Mills vacuum states of the final Schwarzschild black holes, where the n ¼ 1 colored black hole forms the critical solution. The work of Choptuik et al. [Phys. Rev. D 60, 124011 (1999)] is extended by using a family of initial data that includes another region in parameter space where the colored black hole with the opposite sign of the Yang-Mills potential forms the critical solution. We investigate the boundary between the two regions and discover that the Reissner-Nordström solution appears as a new approximate codimension-two attractor.

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Section: Mode Analysismentioning

confidence: 99%

Section: Mode Analysismentioning

confidence: 99%

Section: Mode Analysismentioning

confidence: 99%

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Formation and decay of Einstein-Yang-Mills black holes

Rinne

2014

Phys. Rev. D

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“…However, both the solitons and hairy black holes were soon found to be unstable [11][12][13][14][15][16][17]. Under perturbation, the black holes lose their gauge-field hair and evolve towards a (stable) vacuum black hole solution; the solitons either collapse to form a vacuum black hole or else the gauge field is radiated away to infinity, leaving pure Minkowski spacetime [18][19][20].…”

Section: Introductionmentioning

confidence: 99%

Stability of gravitating charged-scalar solitons in a cavity

2016

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We present new regular solutions of Einstein-charged-scalar-field theory in a cavity. The system is enclosed inside a reflecting mirrorlike boundary, on which the scalar field vanishes. The mirror is placed at the zero of the scalar field closest to the origin, and inside this boundary our solutions are regular. We study the stability of these solitons under linear, spherically symmetric perturbations of the metric, scalar and electromagnetic fields. If the radius of the mirror is sufficiently large, we present numerical evidence for the stability of the solitons. For small mirror radius, some of the solitons are unstable. We discuss the physical interpretation of this instability.

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“…For instance, the gauge group can be enlarged to su(N ) [11][12][13][14][15][16], in which case purely magnetic configurations are described by N − 1 gauge field functions ω j . However, one important property of all the purely magnetic, asymptotically flat, four-dimensional, EYM black holes is that they are dynamically unstable under small perturbations of the metric and gauge field [17][18][19][20][21][22][23].…”

Section: Introductionmentioning

confidence: 99%

Black holes with s u N $$ \mathfrak{s}\mathfrak{u}(N) $$ gauge field hair and superconducting horizons

Shepherd¹,

Winstanley²

2017

J. High Energ. Phys.

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We present new planar dyonic black hole solutions of the su(N ) Einstein-Yang-Mills equations in asymptotically anti-de Sitter space-time, focussing on su(2) and su(3) gauge groups. The magnetic part of the gauge field forms a condensate close to the planar event horizon. We compare the free energy of a non-Abelian hairy black hole with that of an embedded Reissner-Nordström-anti-de Sitter (RN-AdS) black hole having the same Hawking temperature and electric charge. We find that the hairy black holes have lower free energy. We present evidence that there is a phase transition at a critical temperature, above which the only solutions are embedded RN-AdS black holes. At the critical temperature, an RN-AdS black hole can decay into a hairy black hole, and it is thermodynamically favourable to do so. Working in the probe limit, we compute the frequency-dependent conductivity, and find that enlarging the gauge group from su(2) to su(3) eliminates a divergence in the conductivity at nonzero frequency.

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Lifetime of unstable hairy black holes

Cited by 22 publications

References 43 publications

Formation and decay of Einstein-Yang-Mills black holes

Formation and decay of Einstein-Yang-Mills black holes

Stability of gravitating charged-scalar solitons in a cavity

Black holes with s u N $$ \mathfrak{s}\mathfrak{u}(N) $$ gauge field hair and superconducting horizons

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