Instability and new phases of higher-dimensional rotating black holes

Dias, Óscar J. C.; Figueras, Pau; Monteiro, Ricardo; Santos, Jorge E.; Emparan, Roberto

doi:10.1103/physrevd.80.111701

Cited by 148 publications

(228 citation statements)

References 21 publications

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“…This is the first time these corrections have been compared to a numerical solution. Finally, note that in figures 1, 3, 4, 5, and 6, the isolated magenta squares describe the zero modes of the ultraspinning higher harmonics [21,22]. Given our results, we conjecture that two families of lumpy solutions will branch from each of these points, one of which will connect to (possibly lumpy) black saturns or black di-rings etc.…”

Section: Jhep07(2014)045mentioning

confidence: 99%

“…For large rotation, the horizon becomes thin as it spreads along the plane of rotation. These BHs can become unstable to the ultraspinning instability, which is of Gregory-Laflamme type [20][21][22]. It was conjectured that the threshold mode of this instability signals a bifurcation to a new branch of axisymmetric rotating BHs with lumpy or rippled S d−2 horizons.…”

Section: Jhep07(2014)045mentioning

confidence: 99%

“…The solid green line describes the singly spinning MP BH [17]. The large red square indicates the zero mode of the ultraspinning instability [21,22]. Two families of the lumpy BHs (the black squares and brown dots) branch from this zero mode in a second-order phase transition.…”

Section: Jhep07(2014)045mentioning

confidence: 99%

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Rings, ripples, and rotation: connecting black holes to black rings

Dias

Santos

Way

2014

J. High Energ. Phys.

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105

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Singly-spinning Myers-Perry black holes in d ≥ 6 spacetime dimensions are unstable for sufficiently large angular momentum. We numerically construct (in d = 6 and d = 7) two new stationary branches of lumpy (rippled) black hole solutions which bifurcate from the onset of this ultraspinning instability. We give evidence that one of these branches connects through a topology-changing merger to black ring solutions which we also construct numerically. The other branch approaches a solution with large curvature invariants. We are also able to compare the d = 7 ring solutions with results from finite-size corrections to the blackfold approach, finding excellent agreement. JHEP07(2014)045Introduction. As expressed by John Wheeler's statement, "Black holes have no hair" [1], black holes (BHs) in four spacetime dimensions are remarkably simple objects. The topology, rigidity, uniqueness, and no-hair theorems ensure that Kerr BHs are the only stationary, vacuum, and asymptotically flat solutions to general relativity, and that they are uniquely specified by their mass M and angular momentum J [2]. Because Kerr BHs are also linear mode stable [3], any stellar object undergoing gravitational collapse towards a BH is expected to settle to the Kerr solution.Yet, the uniqueness of the Kerr BH may seem surprising given the close connection between gravity and fluids. According to the membrane paradigm [4], external observers will find that BH horizons behave like fluid membranes, endowed with a viscosity, conductivity, temperature, entropy, etc. Moreover, in certain circumstances there are formal mappings between solutions of general relativity and solutions of Navier-Stokes [5,6]. Fluids, however, lack strong uniqueness theorems and admit a rich structure of solutions. Indeed, rotational instabilities appear in fluid droplets and non-spherical solutions develop [7]. In particular, a ring configuration is preferred for high spin. Therefore, it may be natural to suspect that BHs behave like fluid droplets and have a greater diversity of solutions. This is the emerging picture in d > 4 spacetime dimensions.In higher dimensions, gravity becomes weaker as it spreads out over extra dimensions. Horizons are therefore more flexible, creating new gravitational phenomena with no fourdimensional counterparts. For example, in d ≥ 5 black strings exist and suffer from the Gregory-Laflamme instability [8]. This instability leads to a fractal-like array of spherical BHs and cosmic censorship violation [9,10]. This behaviour is similar to the RayleighPlateau instability, where a fluid jet breaks into an array of spherical droplets [11].In addition, there are black rings with horizon topology S 1 × S d−3 . These have been constructed in closed analytic form in d = 5 [12] and numerically in d = 6 [13]. (The list of other BH horizon topologies that are allowed in d > 4 were discussed in [14]). In any d ≥ 5, black rings can be found perturbatively using the blackfold approach if the S 1 radius is much larger than the S d−3 radius [15]...

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Section: Jhep07(2014)045mentioning

confidence: 99%

Section: Jhep07(2014)045mentioning

confidence: 99%

See 1 more Smart Citation

Rings, ripples, and rotation: connecting black holes to black rings

Dias

Santos

Way

2014

J. High Energ. Phys.

Self Cite

105

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“…In particular, they can be unstable [1][2][3][4][5][6], violate black hole uniqueness [2,3,7,8] and also lead to a violation of weak cosmic censorship [9][10][11].…”

Section: Introductionmentioning

confidence: 99%

“…Therefore, for each of these three α's we solve the equations of motion to find f (3,α) i (z) and k (2) . These three systems of equations are independent but k (2) is unique, so we must to get the same k (2) in each of them. This k (2) is presented in (2.16).…”

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confidence: 99%

Lattice black branes: sphere packing in general relativity

Dias

Santos

Way

2018

J. High Energ. Phys.

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Abstract:We perturbatively construct asymptotically R 1,3 × T 2 black branes with multiple inhomogeneous directions and show that some of them are thermodynamically preferred over uniform branes in both the microcanonical and canonical ensembles. This demonstrates that, unlike five-dimensional black strings, the instability of some unstable black branes has a plausible endpoint that does not require a violation of cosmic censorship.

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Instabilities and doubly spinning black holes

Astefanesei

Rodríguez

Theisen

2011

Fortschritte der Physik

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Ultra‐spinning black holes in higher dimensions have qualitatively similar thermodynamical properties to the black strings/p‐branes– they exhibit a black membrane‐like phase. In these notes we will explore which doubly spinning black holes and black rings show this black membrane‐like phase and pinpoint the threshold of these regimes. For the same cases we will study the thermodynamical instabilities in the grand canonical ensemble and compute the zeros of the Hessian of the Gibbs potential. Comparing our results, we will show that the thresholds of the black membrane phase and the thermal instability do not necessarily coincide.

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Instability and new phases of higher-dimensional rotating black holes

Cited by 148 publications

References 21 publications

Rings, ripples, and rotation: connecting black holes to black rings

Rings, ripples, and rotation: connecting black holes to black rings

Lattice black branes: sphere packing in general relativity

Instabilities and doubly spinning black holes

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