Shadow and stability of quantum-corrected black holes

Abstract

Recently the quantum Oppenheimer-Snyder gravitational collapse model has been proposed in loop quantum gravity, providing quantum-corrected Schwarzschild spacetimes as the exterior of the collapsing dust ball. In this paper, the quantum gravity effects on the black hole shadows in this model are studied, and the stability of the quantum-corrected black holes is also analyzed by calculating the quasinormal modes. It turns out that the quantum correction always shrinks the radius of shadows, and the quantum-corrected black holes are stable against the scalar and vector perturbations.

15 pages, 9 figures

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• Shadows and parameter estimation of rotating quantum corrected black holes and constraints from EHT observation of M87* and Sgr A*
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• The instability of the inner horizon of the quantum-corrected black hole
• Spin foam amplitude of the black-to-white hole transition
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• Probing loop quantum effects through solar system experiments: observational signatures and parameter constraints
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• Probing Einstein-Maxwell-Scalar Black hole via Thin Accretion Disks and Shadows with EHT Observations of M87* and Sgr A*
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• Accretion of matter of a new bumblebee black hole
• Black hole images as probes of thermodynamic evolution
• Evolution of interior entropy of a loop quantum-corrected black hole pierced by a cosmic string
• Image of a quantum-corrected black hole without Cauchy horizons illuminated by a static thin accretion disk
• Equatorial periodic orbits and gravitational wave signatures in Euler-Heisenberg black holes surrounded by perfect fluid dark matter