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Abstract
We present a careful study of accelerating black holes in anti-de Sitter spacetime, formulating the thermodynamics and resolving discrepancies that have appeared in previous investigations of the topic. We compute the dual stress-energy tensor for the spacetime and identify the energy density associated with a static observer at infinity. The dual energy-momentum tensor can be written as a three-dimensional perfect fluid plus a non-hydrodynamic contribution with a universal coefficient which is given in gauge theory variables. We demonstrate that both the holographic computation and the method of conformal completion yield the same result for the mass. We compare to previous work on black funnels and droplets, showing that the boundary region can be endowed with non-compact geometry, and comment on this novel holographic dual geometry.
Highlights
We present a careful study of accelerating black holes in anti-de Sitter spacetime, formulating the thermodynamics and resolving discrepancies that have appeared in previous investigations of the topic
We compare to previous work on black funnels and droplets, showing that the boundary region can be endowed with noncompact geometry, and comment on this novel holographic dual geometry
The subject of black hole thermodynamics [1,2,3] has proven to be an invaluable tool to this end, and broad classes of black holes have been shown to exhibit a rich and varied range of thermodynamic behavior, in anti-de Sitter spacetime [4]
Summary
The dual energy-momentum tensor can be written as a three-dimensional perfect fluid plus a nonhydrodynamic contribution with a universal coefficient which is given in gauge theory variables We demonstrate that both the holographic computation and the method of conformal completion yield the same result for the mass. We resolve conflicting issues that exist in the literature, obtain a distinct set of thermodynamic variables that are consistent with the gravitational action, and agree with both the conformal and holographic methods for computing conserved charges To this end, we focus our attention to black holes with no acceleration horizon [15] so that there is no ambiguity as to which horizon temperature should be considered or as to whether there is an equilibrium thermodynamics for the system. We comment on the cases when the acceleration horizons appear and provide a novel interpretation of the boundary geometry
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