Myers–Perry black holes with scalar hair and a mass gap: Unequal spins

Herdeiro, Carlos; Kunz, Jutta; Radu, Eugen; Subagyo, Bintoro Anang

doi:10.1016/j.physletb.2015.06.059

Cited by 54 publications

(42 citation statements)

References 39 publications

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“…At infinity, the decay of the field is still given by (3.16), such that F → 0. Remarkably, the assumption of existence of a power series expansion of F (r) as r → r H implies that, similar to other hairy rotating BH solutions [44,66,67], the synchronization condition…”

Section: The Probe Limit -Skyrmions On a Myers-perry Bh Backgroundmentioning

confidence: 93%

“…One salient feature of these rotating BHs with Skyrme hair is that they possess a static limit. Whereas this is expected, since static BHs with Skyrme hair are known in d = 3 + 1 spacetime dimensions, it contrasts in a qualitative way with the behaviour of other BHs with scalar hair, namely Kerr BHs with scalar hair [44][45][46] or MP BHs with scalar hair [66,67]. It is therefore of some interest to expand on the comparison between these two models, since they are both examples of BHs with scalar hair:…”

Section: Jhep11(2017)037mentioning

confidence: 99%

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Skyrmions, Skyrme stars and black holes with Skyrme hair in five spacetime dimension

Brihaye

Herdeiro

Radu

et al. 2017

J. High Energ. Phys.

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We consider a class of generalizations of the Skyrme model to five spacetime dimensions (d = 5), which is defined in terms of an O(5) sigma model. A special ansatz for the Skyrme field allows angular momentum to be present and equations of motion with a radial dependence only. Using it, we obtain: 1) everywhere regular solutions describing localised energy lumps (Skyrmions); 2) Self-gravitating, asymptotically flat, everywhere non-singular solitonic solutions (Skyrme stars), upon minimally coupling the model to Einstein's gravity; 3) both static and spinning black holes with Skyrme hair, the latter with rotation in two orthogonal planes, with both angular momenta of equal magnitude. In the absence of gravity we present an analytic solution that satisfies a BPS-type bound and explore numerically some of the non-BPS solutions. In the presence of gravity, we contrast the solutions to this model with solutions to a complex scalar field model, namely boson stars and black holes with synchronised hair. Remarkably, even though the two models present key differences, and in particular the Skyrme model allows static hairy black holes, when introducing rotation, the synchronisation condition becomes mandatory, providing further evidence for its generality in obtaining rotating hairy black holes.

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Section: The Probe Limit -Skyrmions On a Myers-perry Bh Backgroundmentioning

confidence: 93%

Section: Jhep11(2017)037mentioning

confidence: 99%

Skyrmions, Skyrme stars and black holes with Skyrme hair in five spacetime dimension

Brihaye

Herdeiro

Radu

et al. 2017

J. High Energ. Phys.

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“…The existence of clouds indicates nonlinear hairy BH solutions [15,32], but the converse needs not be true [45,46]. In order to find such solutions, The vector clouds we have obtained shall be presented in a parameter space spanned by R þ and Ω h , which are defined as [7,47,48] …”

Section: Stationary Vector Cloudsmentioning

confidence: 99%

Maxwell perturbations on Kerr–anti–de Sitter black holes: Quasinormal modes, superradiant instabilities, and vector clouds

Wang

Herdeiro

2016

Phys. Rev. D

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Scalar and gravitational perturbations on Kerr-anti-de Sitter (Kerr-AdS) black holes have been addressed in the literature and have been shown to exhibit a rich phenomenology. In this paper, we complete the analysis of bosonic fields on this background by studying Maxwell perturbations, focusing on superradiant instabilities and vector clouds. For this purpose, we solve the Teukolsky equations numerically, imposing the boundary conditions we have proposed in [1] for the radial Teukolsky equation. As found therein, two Robin boundary conditions can be imposed for Maxwell fields on Kerr-AdS black holes, one of which produces a new set of quasinormal modes even for Schwarzschild-AdS black holes. Here, we show these different boundary conditions produce two different sets of superradiant modes. Interestingly, the "new modes" may be unstable in a larger parameter space. We then study stationary Maxwell clouds that exist at the threshold of the superradiant instability, with the two Robin boundary conditions. These clouds, obtained at the linear level, indicate the existence of a new family of black hole solutions at the nonlinear level, within the Einstein-Maxwell-AdS system, branching off from the KerrNewman-AdS family. As a comparison with the Maxwell clouds, scalar clouds on Kerr-AdS black holes are also studied, and it is shown there are Kerr-AdS black holes that are stable against scalar, but not vector, modes with the same "quantum numbers".

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“…In a recent paper [12], some of us have studied the lensing and shadows of a deformed type of Kerr BHs, known as Kerr BHs with scalar hair (KBHsSH) [54][55][56] (see also [57][58][59][60][61][62][63][64][65][66][67][68][69][70][71] for generalizations and physical properties). These are solutions to Einstein's gravity minimally coupled to a simple and physically reasonable matter content: a complex, massive, free scalar field.…”

Section: Introductionmentioning

confidence: 99%

Chaotic lensing around boson stars and Kerr black holes with scalar hair

et al. 2016

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In a recent paper [P. V. P. Cunha, C. A. R. Herdeiro, E. Radu, and H. F. Runarsson, Phys. Rev. Lett. 115, 211102 (2015).], it was shown that the lensing of light around rotating boson stars and Kerr black holes with scalar hair can exhibit chaotic patterns. Since no separation of variables is known (or expected) for geodesic motion on these backgrounds, we examine the 2D effective potentials for photon trajectories, to obtain a deeper understanding of this phenomenon. We find that the emergence of stable light rings on the background spacetimes allows the formation of "pockets" in one of the effective potentials, for open sets of impact parameters, leading to an effective trapping of some trajectories, dubbed "quasibound orbits." We conclude that pocket formation induces chaotic scattering, although not all chaotic orbits are associated to pockets. These and other features are illustrated in a gallery of examples, obtained with a new ray-tracing code, PYHOLE, which includes tools for a simple, simultaneous visualization of the effective potential, together with the spacetime trajectory, for any given point in a lensing image. An analysis of photon orbits allows us to further establish a positive correlation between photon orbits in chaotic regions and those with more than one turning point in the radial direction; we recall that the latter is not possible around Kerr black holes. Moreover, we observe that the existence of several light rings around a horizon (several fundamental orbits, including a stable one), is a central ingredient for the existence of multiple shadows of a single hairy black hole. We also exhibit the lensing and shadows by Kerr black holes with scalar hair, observed away from the equatorial plane, obtained with PYHOLE.

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Myers–Perry black holes with scalar hair and a mass gap: Unequal spins

Cited by 54 publications

References 39 publications

Skyrmions, Skyrme stars and black holes with Skyrme hair in five spacetime dimension

Skyrmions, Skyrme stars and black holes with Skyrme hair in five spacetime dimension

Maxwell perturbations on Kerr–anti–de Sitter black holes: Quasinormal modes, superradiant instabilities, and vector clouds

Chaotic lensing around boson stars and Kerr black holes with scalar hair

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