Black holes in Einstein-aether theory

By Christian Eling, T. Jacobson. 2006

173 citations recorded by the source corpus.

We study black hole solutions in general relativity coupled to a unit timelike vector field dubbed the ‘aether’. To be causally isolated, a black hole interior must trap matter fields as well as all aether and metric modes. The theory possesses spin-0, spin-1 and spin-2 modes whose speeds depend on four coupling coefficients. We find that the full three-parameter family of local spherically symmetric static solutions is always regular at a metric horizon, but only a two-parameter subset is regular at a spin-0 horizon. Asymptotic flatness imposes another condition, leaving a one-parameter family of regular black holes. These solutions are compared to the Schwarzschild solution using numerical integration for a special class of coupling coefficients. They are very close to Schwarzschild outside the horizon for a wide range of couplings, and have a spacelike singularity inside, but differ inside quantitatively. Some quantities constructed from the metric and aether oscillate in the interior as the singularity is approached. The aether is at rest at spatial infinity and flows into the black hole, but differs significantly from the 4-velocity of freely falling geodesics.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/ecf81e90ac08ef754b10ed6825f5ca4d5d960f23

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. Paolo Pani
2. R. Brito
3. V. Cardoso
4. T. Sotiriou
5. E. Barausse
6. M. Jamil
7. K. Jusufi
8. Qiang Wu

In Nuclear and High Energy Physics

1. R. Brito
2. Paolo Pani
3. V. Cardoso
4. T. Sotiriou
5. E. Barausse
6. M. Jamil
7. K. Jusufi
8. Qiang Wu

Citations in the corpus

• Shadows and deflection angle of charged and slowly rotating black holes in Einstein-Æther theory (2019, methodology): “It is interesting to note that, for the spherically symmetric numerical black hole solution [50] and its representation in the polynomial form [51, 52], one can use (3.”
• Black holes in Einstein-aether and Hořava-Lifshitz gravity (2011, methodology): “[17], to which we refer for a more detailed discussion.”
• Superradiance (2015, background): “orentz-violating theories: nonlinear instabilities A related instability is thought to occur for BHs in Lorentz-violating theories [418,419]. In these theories, BH solutions can exist (see e.g. Refs. [420,421,422] or a recent overview [250]) with multiple, nested horizons, one for each maximal speed”
• Superradiance: Energy Extraction, Black-Hole Bombs and Implications for Astrophysics and Particle Physics (2015, background): “[417, 418, 419] or a recent overview [249]) with multiple, nested horizons, one for each maximal speed of propagation in the theory.”