Instability of ultra-spinning black holes
By Roberto Emparan, R. Myers. 2003
245 citations recorded by the source corpus.
It has long been known that, in higher-dimensional general relativity, there are black hole solutions with an arbitrarily large angular momentum for a fixed mass [1]. We examine the geometry of the event horizon of such ultra-spinning black holes and argue that these solutions become unstable at large enough rotation. Hence we find that higher-dimensional general relativity imposes an effective ``Kerr-bound'' on spinning black holes through a dynamical decay mechanism. Our results also give indications of the existence of new stationary black holes with ``rippled" horizons of spherical topology. We consider various scenarios for the possible decay of ultra-spinning black holes, and finally discuss the implications of our results for black holes in braneworld scenarios.
Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics
View Paper: https://www.semanticscholar.org/paper/ac61403129d56bb3aa3326292f49ef09c643713e
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Citations in the corpus
- The Phase Structure of Higher-Dimensional Black Rings and Black Holes (2007, methodology): “Employing this analogy, we develop further the conjecture in [31] that proposed the existence of ‘pinched’ black holes with spherical topology.”
- Superradiance: Energy Extraction, Black-Hole Bombs and Implications for Astrophysics and Particle Physics (2015, background): “As another example, for D ≥ 6 dimensions where no upper bound on the rotation of Myers-Perry BHs exists, a Gregory-Laflammelike instability renders ultra-spinning BHs unstable [378, 379, 380, 381, 382].”
- GRAVITATIONAL PERTURBATIONS OF HIGHER DIMENSIONAL ROTATING BLACK HOLES (2006, background): “There are arguments suggesting that a Myers-Perry (MP) black hole will be unstable for sufficiently large angular momentum in five [2] and higher [3] dimensions.”
- Black hole chemistry: thermodynamics with Lambda (2016, background): “In four dimensions κS reaches its maximum in the extremal black hole case, while in higher dimensions the ‘softness’ of the equation of state can be used as an indicator of the ultraspinning instability [121].”
- Reentrant phase transitions in rotating anti–de Sitter black holes (2013, background): “For all d ≥ 6 the geometry of a black hole approaches that of a black membrane [22, 23]; setting f = 1− μR the metric is”
- Black Holes in Higher Dimensions (2008, methodology): “A first indication came from the conjecture in [81] of the existence of black holes with spherical horizon topology but with axially-symmetric ‘ripples’ (or ‘pinches’).”
- The large D limit of General Relativity (2013, background): “This is the case even when r0 ' a, in which case rH is very small, the horizon can be highly pancaked (at least if some spins vanish), and rH a, which can be regarded as an ultraspinning limit [27].”
- Gravity and hydrodynamics: lectures on the fluid-gravity correspondence (2009, background): “One encounters for instance Gregory–Laflamme instabilities for black strings and black branes [7] and closely related instabilities for spinning black holes [8].”
- Numerical methods for finding stationary gravitational solutions (2015, methodology): “As pointed out in [397], in d ≥ 5 dimensions the Gregory-Laflamme instability can cause even topologically spherical black holes with highly deformed horizons to break symmetries along their extended directions.”
- Essentials of blackfold dynamics (2009, background): “In a four-dimensional black hole, by virtue of the Kerr bound J ≤ GM2 these lengths are always parametrically similar, but higher-dimensional black holes (including also black rings) with lJ ≫ lM are known to exist in ultra-spinning regimes where the angular momentum for a given mass can be arbitrar”
- Black rings in (Anti)-de Sitter space (2008, background): “In many respects, the limit a→ L and the bound J = M in AdS correspond to the limit a→ ∞ and the ultra-spinning regime of infinite spin for fixed mass of Myers-Perry (MP) black holes [22, 23].”
- A new approach to static numerical relativity and its application to Kaluza–Klein black holes (2009, background): “Whilst these are understood analytically, in D > 5 the black ring solution is not known and it is thought that the structure of stationary solutions is yet more complicated than that in D = 5 [13, 14], with little hope of admitting closed-form solutions.”
- Holographic thermalization, quasinormal modes and superradiance in Kerr-AdS (2013, background): “Indeed, it is established that D ≥ 6 stationary BHs are also unstable to the ultraspinning instability, whose onset was identified in [70] (this instability was first studied in asymptotically flat stationary BHs in D ≥ 6 [71, 72, 73, 67, 74]).”
- An instability of higher-dimensional rotating black holes (2010, methodology): “hould exhibit an instability for suciently large angular momentum. The MP solution is parameterized by its mass M and b(D 1)=2cangular momenta (where bcstands for the smallest integer part). In Ref. [8], it was shown that if only one angular momentum is non-vanishing then, in the limit in which this”