Quasinormal modes of a holonomy corrected Schwarzschild black hole

Moreira, Zeus S.; Lima, Haroldo C. D.; Crispino, Luís C. B.; Herdeiro, Carlos

doi:10.1103/physrevd.107.104016

Cited by 16 publications

(1 citation statement)

References 56 publications

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“…However, finding solutions in the scope of the full theory is a difficult task, and some effective models have been considered in the search for non-singular black holes. These make use of the polymerisation of classical Hamiltonians, which gives origin to a transition hypersurface in the horizon inner region, at which a tunneling from a black hole to a white hole takes place [11][12][13][14][15][16][17][18][19][20][21][22].…”

Section: Introductionmentioning

confidence: 99%

Remnant loop quantum black holes

Borges,

Baranov,

Sobrinho

et al. 2024

Class. Quantum Grav.

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Polymer models inspired by Loop Quantum Gravity (LQG) have been used to describe non-singular quantum black holes with spherical symmetry, with the classical singularity replaced by a transition from a black hole to a white hole. A recent model, with a single polymerisation parameter, leads to a symmetric transition with same mass for the black and white phases, and to an asymptotically flat exterior metric. The radius of the transition surface is, however, not fixed, increasing with the mass. Following similar procedures, in a previous paper we have fixed that radius by identifying the minimal area on the transition surface with the area gap of LQG. This allowed to find a dependence of the polymerisation parameter on the black hole mass, with the former increasing as the latter decreases. It also permitted to extend the model to Planck scale black holes, with quantum fluctuations remaining small at the horizon. In the present paper we extend this analysis to charged black holes, showing that the Cauchy horizon lies beyond of the transition surface. We also show the existence of limiting states with zero surface gravity, the lightest one with $Q = 0$ and $m = \sqrt{2}/4$, and the heaviest with $Q = m = \sqrt{2}/2$. Using our solutions to approximate quasi-steady horizons, we show that Hawking evaporation leads asymptotically to these extremal states, leaving remnant black holes of Planck size.

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Section: Introductionmentioning

confidence: 99%

Remnant loop quantum black holes

Borges,

Baranov,

Sobrinho

et al. 2024

Class. Quantum Grav.

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Scalar Quasi-Normal Modes of a loop quantum black hole

Livine,

Montagnon,

Oshita

et al. 2024

J. Cosmol. Astropart. Phys.

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We compute the Quasi-Normal Mode (QNM) frequencies for scalar perturbations for modified Schwarzschild black holes in Loop Quantum Gravity. We study the singularity-free polymerized metric characterized by two parameters encoding loop quantum effects: the minimal area gap a 0 and the polymeric deformation parameter P. We perform numerical computations using Leaver's continued fraction method and compare our results to other semi-analytical methods and existing literature. We study the effects on the QNM spectrum of variation of both deformation parameters and systematically compare to the standard Schwarzschild case. In particular we find that the scalar fundamental mode is modified from the third decimal for values of P in accordance with the most recent astrophysical constraints. We also show that qualitative differences arise for highly damped modes: on the one hand, a new crossing of the imaginary axis occurs for high values of a 0 and, on the other hand, increasing P produces a positive shift of the real part and an increase of the spacing in imaginary part between modes.

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