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Towards thermodynamics of universal horizons in Einstein-{\ae}ther theory

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arxiv 1210.4940 v2 pith:HNZVR55P submitted 2012-10-17 hep-th gr-qc

Per Berglund , Jishnu Bhattacharyya , David Mattingly This is my paper · ORCID
classification hep-thgr-qc
keywords causalhorizonstheoryuniversalblackeinstein-fieldgeneral
verification ladder T0 review T1 audit T2 compute T3 formal
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Holography grew out of black hole thermodynamics, which relies on the causal structure and general covariance of general relativity. In Einstein-{\ae}ther theory, a generally covariant theory with a dynamical timelike unit vector, every solution breaks local Lorentz invariance, thereby grossly modifying the causal structure of gravity. However, there are still absolute causal boundaries, called "universal horizons", which are not Killing horizons yet obey a first law of black hole mechanics and must have an entropy if they do not violate a generalized second law. We couple a scalar field to the timelike vector and show via the tunneling approach that the universal horizon radiates as a blackbody at a fixed temperature, even if the scalar field equations also violate local Lorentz invariance. This suggests that the class of holographic theories may be much broader than currently assumed.

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Cited by 3 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Revisit Static Aether: Exact Vacuum Solution in Einstein-Aether Theory and Its Analytic Extension

    gr-qc 2026-06 unverdicted novelty 6.0 of 10

    Exact static vacuum solution in Einstein-Aether theory parameterized by c14, with analytic extension showing naked singularities or wormhole geometries rather than black holes when c14 is nonzero.

  2. Einstein-aether Elliptic Charges and the First Law of Asymptotically AdS Black Holes

    gr-qc 2026-06 unverdicted novelty 6.0 of 10

    Einstein-aether theory admits an elliptic charge arising from a symmetry of the reduced action that explains the misalignment contribution to the first law for asymptotically AdS universal horizons.

  3. Quasinormal Modes and Dynamical Evolution of Scalar Fields in the Einstein-Bumblebee Theory with a Cosmological Constant

    gr-qc 2025-02 conditional novelty 4.0 of 10

    For scalar perturbations of Einstein-Bumblebee black holes in de Sitter spacetime, increasing the Lorentz-violation parameter or the cosmological constant generally lowers the quasinormal mode frequency and damping rate.

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