Vortex hair on AdS black holes

Abstract

We analyse vortex hair for charged rotating asymptotically AdS black holes in the abelian Higgs model. We give analytical and numerical arguments to show how the vortex interacts with the horizon of the black hole, and how the solution extends to the boundary. The solution is very close to the corresponding asymptotically flat vortex, once one transforms to a frame that is non-rotating at the boundary. We show that there is a Meissner effect for extremal black holes, with the vortex flux being expelled from sufficiently small black holes. The phase transition is shown to be first order in the presence of rotation, but second order without rotation. We comment on applications to holography.Comment: 24 pages, 7 figures, references adde

Black hole thermodynamics with conical defects

“…Even for the non-accelerating rotating black hole, the thermodynamics are more subtle, requiring an adjustment of the angular velocity [40] in order to define it relative to a non-rotating frame at infinity. For a conical defect running through the black hole (though see [62,63] for a full discussion of subtleties of replacing deficits by finite width defects) one can follow the method of section 2 to generalise the appropriate thermodynamical variables of Gibbons et al [40] where K is the (arbitrary) parameter determining the periodicity of the azimuthal angle as before, and L is a new parameter due to black hole rotation:…”

Are “Superentropic” black holes superentropic?

“…In a physical picture, one might think about such a conical deficit as being caused by a cosmic string threading the black hole, though it is not entirely clear that this is a complete story for rotating black holes[28,29].…”

Accelerating black hole chemistry

“…While it is possible for material systems to have many charges and chemical potentials, the black hole on the other hand is believed to carry only mass, charge and angular momentum, a situation summed up by the no-hair theorems [11,12], and while these are now understood in a broader context to be somewhat limited, the basic picture from the perspective of classic black hole thermodynamics was that thermodynamic charges were still narrowly restricted, M = M(S, P, J, Q). Recently however, a new type of 'charge' for a black hole has been explored and added to this stable: a conical deficit, µ [13][14][15][16][17], often interpreted as a cosmic string, that can either run symmetrically along the axis of the black hole [18][19][20][21], or have different values along the North and South axes, leading to an accelerating black hole, encoded by the C-metric [22,23] (and including a negative cosmological constant Λ = −3/ℓ 2 ):…”