The Phase Structure of Higher-Dimensional Black Rings and Black Holes

By Roberto Emparan, T. Harmark, V. Niarchos, N. Obers, Maria J Rodriguez. 2007

199 citations recorded by the source corpus.

We construct an approximate solution for an asymptotically flat, neutral, thin rotating black ring in any dimension D ≥ 5 by matching the near-horizon solution for a bent boosted black string, to a linearized gravity solution away from the horizon. The rotating black ring solution has a regular horizon of topology S1 × SD−3 and incorporates the balancing condition of the ring as a zero-tension condition. For D = 5 our method reproduces the thin ring limit of the exact black ring solution. For D ≥ 6 we show that the black ring has a higher entropy than the Myers-Perry black hole in the ultra-spinning regime. By exploiting the correspondence between ultra-spinning black holes and black membranes on a two-torus, we take steps towards qualitatively completing the phase diagram of rotating blackfolds with a single angular momentum. We are led to propose a connection between MP black holes and black rings, and between MP black holes and black Saturns, through merger transitions involving two kinds of `pinched' black holes. More generally, the analogy suggests an infinite number of pinched black holes of spherical topology leading to a complicated pattern of connections and mergers between phases.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/6100afb31ba03cac917d70de1f2be6414e3ac35d

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Citations in the corpus

Essentials of blackfold dynamics (2009, methodology): “For higher-dimensional black rings these first corrections have been computed [6].”
Black Holes in Higher Dimensions (2008, methodology): “Nevertheless, [80] contains advanced heuristic arguments, which propose a completion of the curves that is qualitatively consistent with all the information available at present.”
Bicycling black rings (2007, methodology): “Recently the matched asymptotic expansion method was used to construct large radius higher dimensional black rings [38].”
Numerical methods for finding stationary gravitational solutions (2015, background): “These include the matched asymptotic expansion [37]; the non-interacting thermodynamical model and the higher order matched asymptotic expansion for nonlinear solutions [38–45]; the fluid/gravity correspondence (a long-wavelength gradient expansion) [46, 47] reviewed in [27, 48]; the blackfold appro”
Black rings in (Anti)-de Sitter space (2008, background): “For d ≥ 6 they are very likely correct up to the next order: in the same way as argued in [4], the dipole corrections to the metric induced at order r0/min (R,L) do not generate any corrections to the physical magnitudes.”
A new approach to static numerical relativity and its application to Kaluza–Klein black holes (2009, background): “rn’ [11,12]. 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 in D= 5 [13,14], with little hope of admitting closed-form solutions. Now consider Kaluza-Klein theory, by w”