Running Newton Coupling, Scale Identification and Black Hole Thermodynamics
arXiv:2204.09892 · doi:10.1103/PhysRevD.105.106026
Abstract
We discuss the quantum improvement of black hole solutions in the context of asymptotic safety. The Newton coupling in this formulation depends on an energy scale, which must be identified with some length scale in order to study physical consequences to black holes. However, no physical principle has so far been known for the identification. Here we propose that the consistency of the first law of thermodynamics is the principle that should determine physically sensible scale identification, at least close to the horizon. We show that this leads to a natural solution that the Newton coupling should be a function of the horizon area and find a universal formula for the quantum entropy, which agrees with the standard Bekenstein-Hawking entropy for constant Newton coupling, for Kerr black holes and other higher-dimensional black holes. This suggests that the Newton coupling is a function of the area near the horizon, and also away to infinity, where the quantum effects may not be so important.
arXiv comment14 pages, v2: various elaborations, 2 refs. added
References in corpus (24)
- Formation and evaporation of non-singular black holes
- Nonperturbative Evolution Equation for Quantum Gravity
- Black hole entropy in Loop Quantum Gravity
- Logarithmic correction to the Bekenstein-Hawking entropy
- Renormalization group improved black hole spacetimes
- Non-Trivial Ultraviolet Fixed Point in Quantum Gravity
- Spacetime Structure of an Evaporating Black Hole in Quantum Gravity
- Instabilities of Black Strings and Branes
- QED coupled to QEG
- Running Newton Constant, Improved Gravitational Actions, and Galaxy Rotation Curves
- A Critique of the Asymptotic Safety Program
- Black holes and asymptotically safe gravity
- Black holes within Asymptotic Safety
- Structural aspects of asymptotically safe black holes
- Quantum Gravity Effects in the Kerr Spacetime
- Black hole thermodynamics under the microscope
- From renormalization group flows to cosmology
- Quantum Improved Schwarzschild-(A)dS and Kerr-(A)dS Space-times
- From a locality-principle for new physics to image features of regular spinning black holes with disks
- Gravitational collapse in Quantum Einstein Gravity
- Quantum improved charged black holes
- Stresses and Strains in the First Law for Kaluza-Klein Black Holes
- Quantum gravity effects in Myers-Perry space-times
- Non-Perturbative Quantum Correction to the Reissner-Nordström spacetime with Running Newton's Constant
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- Effective action and black hole solutions in asymptotically safe quantum gravity
- Generalized Entropy Implies Varying-G: Horizon Area Dependent Field Equations and Black Hole-Cosmology Coupling
- Hawking radiation of renormalization group improved regular black holes
- Effective geometrodynamics for renormalization-group improved black-hole spacetimes in spherical symmetry
- Image of Quantum Improved Regular Kerr Black Hole and Parameter Constraints from EHT Observations
- Regular black hole from a confined spin connection in Poincare gauge gravity
- GUP Effective Metric Without GUP: Implications for the Sign of GUP Parameter and Quantum Bounce
- Evaporation of a nonsingular Reissner-Nordström black hole and information loss problem
- Do Black Holes With Generalized Entropy Violate Bekenstein Bound?
- Equivalence of scalar-tensor theories and scale-dependent gravity
- Shadow of rotating black holes with consistent thermodynamics
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