Abstract
Using the Wald formalism, we investigate the thermodynamics of charged black holes in D-dimensional stationary spacetimes with or without rotations in Einstein-æther–Maxwell theory. In particular, assuming the existence of a scaling symmetry of the action, we obtain the Smarr integral formula, which can be applied to both Killing and universal horizons. When restricted to 4-dimensional spherically symmetric spacetimes, previous results obtained by a different method are re-derived.
Highlights
Jacobson and Mattingly introduced a unit time-like 4-vector field ua, the so-called “æther field” coupled to Einstein’s general relativity (GR), which is often referred to as the Einsteinæther theory [1]
It was shown that the universal horizon radiates still as a blackbody at a fixed temperature, but remarkably it depends on z [12], and Landau-Lifshitz pseudo-tensors [24], while Foster investigated the same problem by using the Wald formalism [25]
In this letter, using the Wald formalism, we investigate the thermodynamics of charged black holes in D-dimensional stationary spacetimes with or without rotations in Einstein-ætherMaxwell theory
Summary
Jacobson and Mattingly introduced a unit time-like 4-vector field ua, the so-called “æther field” coupled to Einstein’s general relativity (GR), which is often referred to as the Einsteinæther theory [1]. It was shown that the universal horizon radiates still as a blackbody at a fixed temperature, but remarkably it depends on z [12], and Landau-Lifshitz pseudo-tensors [24], while Foster investigated the same problem by using the Wald formalism [25] From their expressions, one can deduce the ADM mass in asymptotically flat spacetimes with a modification due to the presence of the æther field. Assuming the existence of a scaling symmetry of the action [14], we obtain the Smarr integral formula, which can be applied to both Killing and universal horizons.
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