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The phase diagram of Einstein-Weyl gravity
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Thanks to their interpretation as first order correction of General Relativity at high energies, quadratic theories of gravity gained much attention in recent times. Particular attention has been drawn to the Einstein-Weyl theory, where the addition of the squared Weyl tensor to the action opens the possibility of having non-Schwarzschild black holes in the classical spectrum of the theory. Static and spherically symmetric solutions of this theory have been studied and classified in terms of their small scales behaviour; however, a classification of these solutions in terms of the asymptotic gravitational field is still lacking. In this paper we address this point and present a phase diagram of the theory, where the different types of solutions are shown in terms of their mass and the strength of a Yukawa-like correction to the gravitational field. In particular we will show that, in the case of compact stars, different equations of state imply different Yukawa corrections to the gravitational potential, with possible phenomenological implications.
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Cited by 5 Pith papers
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Spherically symmetric solutions in quasi-local Einstein-Weyl gravity
In quasi-local Einstein-Weyl gravity, static spherically symmetric Frobenius solutions are classified: regular cores only, Schwarzschild-like horizons and wormhole throats, plus asymptotic 1/r^6 corrections to Schwarzschild.
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Rotating near-horizon extreme geometries in quadratic gravity
New regular Bachian near-horizon extreme geometries are found in Einstein-Weyl gravity, and their horizon area is bounded above, suggesting microscopic extremal rotating black holes.
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Time Evolution of Black Hole Perturbations in Quadratic Gravity
Gravitational perturbations of Einstein-Weyl black holes show late-time oscillatory tails decaying as t^{-5/6} and break the null-geodesic correspondence in the eikonal regime.
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Charting GLOBs in Asymptotically Safe Gravity
Within the Einstein-Weyl truncation, asymptotically safe gravity predicts a Weyl coefficient m_2 = 1.4 m_Pl, which constrains the phase diagram of compact objects: attractive naked singularities are disfavored while w...
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Ghost-induced phase transition in the final stages of black hole evaporation
A quantum ghost instability is claimed to send evaporating Schwarzschild black holes to stable naked singularities, merging the information paradox with the singularity problem.
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