Coherent quantum state corrections in RN--black holes: Photon dynamics, shadow casts, and energy backreaction
Abstract
We revisit the Reissner-Nordström (RN) geometry within the coherent quantum black hole framework, introducing a version that remains well-behaved at short distances while preserving the expected classical behavior at large scales. The key ingredient is a smooth Gaussian regularization, which replaces the usual sharp cutoff and {suppresses} the unphysical oscillations. This construction introduces a characteristic core radius Rs, constrained relative to the mass M and charge Q to ensure either a {Ricci-regular} center or a softened integrable singularity. Near the origin, the spacetime exhibits distinct behaviors depending on the choice of parameters. When Rs satisfies the critical relation Rs* = √π RQ2 / RM, the geometry is {Ricci-regulFar}, while deviations from this value produce a milder, integrable singularity. {We clarify that for generic parameters, the Kretschmann scalar retains a 1/r divergence even at Rs*, so the center is not fully regular in the sense of finite curvature invariants.} The effective stress-energy tensor can be interpreted as an anisotropic fluid, whose density and pressure smoothly interpolate between the quantum-dominated core and the classical RN region at large radii. The Misner-Sharp mass accumulates gradually from the center, recovering the ADM mass asymptotically. The quantum scale also modifies the horizon structure, giving rise to standard, extremal, or horizonless configurations depending on the ratios α=RQ/RM and β=Rs/RM. Photon motion is correspondingly affected: the photon sphere moves inward, light deflection and Shapiro delay are slightly reduced, and the resulting shadow appears more compact and smoother, reflecting the quantum-corrected geometry.
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BibTeX
@misc{errehymy2026coherent,
title = {{Coherent quantum state corrections in RN--black holes: Photon dynamics, shadow casts, and energy backreaction}},
author = {A. Errehymy and Y. Khedif and M. Daoud and B. Turimov and S. Usanov and Z. Yasakov and F. Turaev},
howpublished = {arXiv},
year = {2026},
month = oct,
doi = {10.48550/arxiv.2610.03777},
eprint = {2610.03777},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2610.03777},
}
RIS
TY - UNPB
TI - Coherent quantum state corrections in RN--black holes: Photon dynamics, shadow casts, and energy backreaction
AU - A. Errehymy
AU - Y. Khedif
AU - M. Daoud
AU - B. Turimov
AU - S. Usanov
AU - Z. Yasakov
AU - F. Turaev
PY - 2026
DA - 2026/10/01
PB - arXiv
DO - 10.48550/arxiv.2610.03777
UR - https://arxiv.org/abs/2610.03777
AB - We revisit the Reissner-Nordström (RN) geometry within the coherent quantum black hole framework, introducing a version that remains well-behaved at short distances while preserving the expected classical behavior at large scales. The key ingredient is a smooth Gaussian regularization, which replaces the usual sharp cutoff and {suppresses} the unphysical oscillations. This construction introduces a characteristic core radius R_s, constrained relative to the mass M and charge Q to ensure either a {Ricci-regular} center or a softened integrable singularity. Near the origin, the spacetime exhibits distinct behaviors depending on the choice of parameters. When R_s satisfies the critical relation R_s^* = √π R_Q^2 / R_M, the geometry is {Ricci-regulFar}, while deviations from this value produce a milder, integrable singularity. {We clarify that for generic parameters, the Kretschmann scalar retains a 1/r divergence even at R_s^*, so the center is not fully regular in the sense of finite curvature invariants.} The effective stress-energy tensor can be interpreted as an anisotropic fluid, whose density and pressure smoothly interpolate between the quantum-dominated core and the classical RN region at large radii. The Misner-Sharp mass accumulates gradually from the center, recovering the ADM mass asymptotically. The quantum scale also modifies the horizon structure, giving rise to standard, extremal, or horizonless configurations depending on the ratios α=R_Q/R_M and β=R_s/R_M. Photon motion is correspondingly affected: the photon sphere moves inward, light deflection and Shapiro delay are slightly reduced, and the resulting shadow appears more compact and smoother, reflecting the quantum-corrected geometry.
ER -