The evolution of unstable black holes in anti-de Sitter space

By S. Gubser, Indrajit Mitra. 2000

338 citations recorded by the source corpus.

We examine the thermodynamic stability of large black holes in four-dimensional anti-de Sitter space, and we demonstrate numerically that black holes which lack local thermodynamic stability often also lack stability against small perturbations. This shows that no-hair theorems do not apply in anti-de Sitter space. A heuristic argument, based on thermodynamics only, suggests that if there are any violations of Cosmic Censorship in the evolution of unstable black holes in anti-de Sitter space, they are beyond the reach of a perturbative analysis.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/1f299a7125ebbf3852a145bed0d22d506a7cc60f

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Citations in the corpus

An instability of higher-dimensional rotating black holes (2010, methodology): “, this correspondence between the threshold unstable mode and a Euclidean negative mode of the black hole was used in Ref. [31] to justify the Gubser-Mitra conjecture regarding black string stability [15, 16]. In the present context, this conjecture asserts that a black string with a non-compact z-d”
Numerical methods for finding stationary gravitational solutions (2015, background): “[565] S.”
Black Holes in Higher Dimensions (2008, background): “These black holes exhibit an interesting instability [121, 122].”
Signature of the Van der Waals like small-large charged AdS black hole phase transition in quasinormal modes (2014, background): “In AdS black holes, thermodynamic phase transition in the dual field theory corresponds to the onset of instability of a black hole, so that quasinormal modes of black holes are naturally connected with thermodynamic phase transitions of strongly coupled field theories [49].”
A holographic critical point (2010, background): “Precisely for T = Tc the curve will cease to be multivalued, as the three solutions coalesce into one; the curve ρ(μ) will have an infinite slope, indicating (9)According to the correlated stability conjecture (CSC) [24, 25], such black hole solutions will also have dynamical instabilities, correspo”
Mimicking the QCD equation of state with a dual black hole (2008, background): “However, the CSC remains a conjecture, and there appears to be room for violations: see for example [23, 24, 25].”
Landscape of superconducting membranes (2009, background): “(10)There is another known instability for the case of M7 = S (7), the Gubser-Mitra instability [53, 54].”
The phase transition between caged black holes and black strings (2004, background): “ough our “basic vertex”: a stable large black hole and an unstable small black hole, but thermal AdS still has lower free energy. Here we are assuming the Gubser-Mitra Correlated Stability Conjecture [36, 37] to infer the perturbative stability or instability from the sign of the speciﬁc heat and th”
Black hole bound states in AdS(3) x S**2 (2008, background): “Related thermodynamical as well as dynamical instabilities were studied among others in [6, 7, 8, 9, 10, 11, 12, 13, 14, 15].”
GRAVITATIONAL PERTURBATIONS OF HIGHER DIMENSIONAL ROTATING BLACK HOLES (2006, background): “However, this proof has been criticized [34] because it assumes the dominant energy condition, which is violated if μ2 < 0.”
Phase Diagram of N=4 Super-Yang-Mills Theory with R-Symmetry Chemical Potentials (2006, neutral): “For the case of the RN-AdS black hole in four dimensions, Gubser and Mitra [19] found that the instability point is almost exactly where supergravity develops tachyonic modes.”