The phase transition between caged black holes and black strings
By B. Kol. 2004
177 citations recorded by the source corpus.
Abstract Black-hole uniqueness is known to fail in higher dimensions, and the multiplicity of black hole phases leads to phase transitions physics in General Relativity. The black-hole black-string transition is a prime realization of such a system and its phase diagram has been the subject of considerable study in the last few years. The most surprising results seem to be the appearance of critical dimensions where the qualitative behavior of the system changes, and a novel kind of topology change. Recently, a full phase diagram was determined numerically, confirming earlier predictions for a merger of the black-hole and black-string phases and giving very strong evidence that the end-state of the Gregory–Laflamme instability is a black hole (in the dimension range 5 ⩽ D ⩽ 13 ). Here this progress is reviewed, illustrated with figures, put into a wider context, and the still open questions are listed.
Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics
View Paper: https://www.semanticscholar.org/paper/9c68a2dcba3791433597b7f28c7bdd6d0e4f4ef7
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Citations in the corpus
- Non-relativistic gravitation: from Newton to Einstein and back (2007, methodology): “Caged black holes were previously analyzed by means of Matched Asymptotic Expansion (MAE) [3, 4, 5, 6] due to their part in the black-hole black-string phase transition [7, 8, 9] associated with the black string instability of Gregory-Laflamme [10].”
- Mimicking the QCD equation of state with a dual black hole (2008, background): “Considerable work has been devoted to the question of what the endpoint of the evolution of the Gregory-Laflamme instability might be: see for example [26, 27, 28, 29, 30, 31].”
- A new approach to static numerical relativity and its application to Kaluza–Klein black holes (2009, methodology): “The method has been used effectively in a variety of contexts [36–43], but is fundamentally limited in that it requires cohomogenity 2, a particular conformal coordinate system, and a certain ‘wizardry’ in actually making it work—for example, the ‘trick’ employed when treating a symmetry axis [15, 2”
- Black Holes in Higher Dimensions (2008, background): “The instabilities of black strings and black branes [118, 119] have been reviewed in [167, 128], so we shall be brief in this section and only mention the features that are most relevant to our subject.”