Simpson-Visser regularization of the quantum Oppenheimer-Snyder-Datt black hole
Abstract
We study the spherical geometry from the Simpson-Visser prescription r→√(r2+a2) to the quantum Oppenheimer-Snyder-Datt (qOSD) black hole of loop quantum cosmology, whose lapse function A=1−2M/R+αM2/R4 carries the correction α. This family interpolates between the qOSD black hole (a→0), the Simpson-Visser black bounce (α→0), and Schwarzschild. The geometry is regular for every a>0, the Ricci scalar at the throat is blind to α while the Kretschmann scalar is not, and the null energy condition is violated at the throat by −1/(4πa2). The (α,a) plane splits into a two-horizon regular black hole, a single-horizon black hole with a hidden bounce, no Cauchy horizon, and a traversable wormhole; the middle region removes the mass-inflation channel of regular black holes without fine tuning. Because circular orbits are governed by the areal radius, photon sphere, shadow, ISCO and azimuthal epicyclic frequency depend on α only, whereas the Lyapunov exponent and radial epicyclic frequency carry the factor √(1−a2/R2): shadow constrains only α, while ringdown damping and the twin-peak quasiperiodic-oscillation ratio are sensitive to a. We derive horizon thermodynamics with a first-law entropy that departs from the area law, show that the bounce changes the thermodynamic topological charge from W=−1 to W=0 at every α, and compute scalar, electromagnetic and Dirac quasinormal spectra using third-order WKB, Chebyshev spectral collocation and time-domain integration, which agree with one another and with eikonal scaling. Greybody bounds, Hawking emission, cascade sparsity and ringdown quality factor complete the analysis, and in the wormhole region the double-peaked potential produces echoes.
Related
- Observational properties of magnetized quantum Oppenheimer-Snyder black holes
- Naked Singularities and Black Hole Thermodynamics from Shadows and Photon Rings in the Quantum Oppenheimer-Snyder Model
- Canonical-Ensemble Stability of the Quantum Oppenheimer-Snyder Black-Hole Exterior
- Tidal forces in the quantum Oppenheimer--Snyder black hole
- Joint Constraints on Quantum Oppenheimer--Snyder Black Holes from High-Frequency Quasi-Periodic Oscillations in X-ray Binary Systems and the S2 Star Orbit
BibTeX
@misc{ahmed2026simpsonvisser,
title = {{Simpson-Visser regularization of the quantum Oppenheimer-Snyder-Datt black hole}},
author = {Faizuddin Ahmed and Ahmad Al-Badawi and İzzet Sakallı},
howpublished = {arXiv},
year = {2026},
month = oct,
doi = {10.48550/arxiv.2610.02266},
eprint = {2610.02266},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2610.02266},
note = {CC BY 4.0},
}
RIS
TY - UNPB
TI - Simpson-Visser regularization of the quantum Oppenheimer-Snyder-Datt black hole
AU - Faizuddin Ahmed
AU - Ahmad Al-Badawi
AU - İzzet Sakallı
PY - 2026
DA - 2026/10/01
PB - arXiv
DO - 10.48550/arxiv.2610.02266
UR - https://arxiv.org/abs/2610.02266
AB - We study the spherical geometry from the Simpson-Visser prescription r→√(r^2+a^2) to the quantum Oppenheimer-Snyder-Datt (qOSD) black hole of loop quantum cosmology, whose lapse function A=1−2M/R+αM^2/R^4 carries the correction α. This family interpolates between the qOSD black hole (a→0), the Simpson-Visser black bounce (α→0), and Schwarzschild. The geometry is regular for every a>0, the Ricci scalar at the throat is blind to α while the Kretschmann scalar is not, and the null energy condition is violated at the throat by −1/(4πa^2). The (α,a) plane splits into a two-horizon regular black hole, a single-horizon black hole with a hidden bounce, no Cauchy horizon, and a traversable wormhole; the middle region removes the mass-inflation channel of regular black holes without fine tuning. Because circular orbits are governed by the areal radius, photon sphere, shadow, ISCO and azimuthal epicyclic frequency depend on α only, whereas the Lyapunov exponent and radial epicyclic frequency carry the factor √(1−a^2/R^2): shadow constrains only α, while ringdown damping and the twin-peak quasiperiodic-oscillation ratio are sensitive to a. We derive horizon thermodynamics with a first-law entropy that departs from the area law, show that the bounce changes the thermodynamic topological charge from W=−1 to W=0 at every α, and compute scalar, electromagnetic and Dirac quasinormal spectra using third-order WKB, Chebyshev spectral collocation and time-domain integration, which agree with one another and with eikonal scaling. Greybody bounds, Hawking emission, cascade sparsity and ringdown quality factor complete the analysis, and in the wormhole region the double-peaked potential produces echoes.
ER -