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Vacuum spherically symmetric loop quantum gravity in the midi-superspace approximation using inhomogeneous horizon-penetrating slices has been studied for a decade, and it has been noted that the singularity is eliminated. It is replaced by a region of high curvature and potentially large quantum fluctuations. It was recently pointed out that the effective semiclassical metric implies the existence of a shell of matter which violates energy conditions in regions where the curvature is largest. Here, we propose an alternative way of treating the problem that is free from the shells. The ambiguity in the treatment is related with the existence of new observables in the quantum theory that characterize the area excitations, and how the counterpart of diffeomorphisms in the discrete quantum theory is mapped to the continuum semiclassical picture. The resulting spacetime in the high curvature region inside the horizon is approximated by a metric of the type of the Simpson–Visser wormhole and it connects the black hole interior to a white hole in a smooth manner. [ABSTRACT FROM AUTHOR]

Recently, thermodynamics has given an important aspect of black hole physics, and it is being used as a solemn tool in characterizing the physicality and viability of many black hole (BH) solutions. On the other hand, Heisenberg algebraic deformations, which predict a lower bound to position and/or momentum, are interrogated to have a theory of quantum gravity. In this paper, we consider a combined deformation of the generalized uncertainty and extended generalized uncertainty principles (EGUP) and investigate the EGUP-corrected thermal quantities of the rotating charged BTZ BH. [ABSTRACT FROM AUTHOR]

Astrophysical objects and the surrounding geometry must be described by suitable states in the complete quantum theory of matter and gravity. We attempt at reconstructing such a state for a Schwarzschild black hole from the analysis of a collapsing ball of dust and describing the outer geometry by means of a coherent state. [ABSTRACT FROM AUTHOR]

One of the foremost goals of theoretical modern physics is to obtain a reliable theory of quantum gravity. In so doing, new fundamental scales are being proposed. For example, in the Snyder–de Sitter (SdS) model, two scales manifest which relate measurement limits of the position and momentum. In this work, we study the thermodynamic functions of the Schwarzschild black hole in the SdS model within the presence of position independent and dependent gravity's rainbow. Heuristically, we prove the presence of a nonzero lower bound value of the horizon, mass and temperature of the black hole. Then, we present the stability and remnant conditions of the black hole according to the entropy and heat capacity functions. [ABSTRACT FROM AUTHOR]

In this paper, we consider the theory of infinitely extended particles as the quantum theory of gravity, which unifies all fundamental interactions. We write the space–time metric, which is Schwarzschild-like black hole. We calculate Hamiltonian and Lagrangian, and from these, we obtain the potential energy and study the polymer quantization. We construct effective potential and discuss the gravitational wave of this theory. Also, we study the geodesic motion of a particle near the black hole. Finally, we analyze the apparent shape, radius and distortion of the shadow of the black hole. [ABSTRACT FROM AUTHOR]

Classical black holes shield us from the singularities that inevitably appear in general relativity. Singularity regularization being one of the main landmarks for a successful theory of quantum gravity, quantum black holes are not obliged to hide their inner core from the outside world. Notwithstanding the aforesaid, it is often implicitly assumed that quantum gravity effects must remain confined to black hole interiors. In this essay, we argue in the opposite direction, discussing theoretical evidence for the existence of strong correlations between the physics inside and outside nonsingular black holes. We conclude that astronomical tests of the surroundings of black holes can provide invaluable information about their so-far unexplored interiors. [ABSTRACT FROM AUTHOR]

The motivation behind this study is to enumerate the leading order corrections to the thermodynamics of BTZ black hole (named after three scientists; Banados, Teitelboim, and Zanelli). We first analyze the effect of quantum corrections (motivated from string theory and loop quantum gravity) on various thermodynamic variables for uncharged and stationary BTZ black hole. We, later on, endow charges and rotations to the same black hole and rederive all the expressions once again. The comparative analysis is done between the corrected and uncorrected thermodynamics via plots. [ABSTRACT FROM AUTHOR]

We argue that, when certain higher-curvature corrections are added to the four-dimensional Einstein-Hilbert action, black holes become stable below certain mass. We show this to be the case for an infinite family of ghost-free theories involving terms of arbitrarily high order in curvature. The thermodynamic behavior of the new black holes is universal for arbitrary values of the couplings, with the only exception of the Schwarzschild solution itself, which is recovered when all the couplings are set to zero. For this class of theories, the issue of non-unitary evolution is inexistent, as black holes never evaporate completely. [ABSTRACT FROM AUTHOR]