Joint Constraints on Quantum Oppenheimer--Snyder Black Holes from High-Frequency Quasi-Periodic Oscillations in X-ray Binary Systems and the S2 Star Orbit
Abstract
We study a quantum-corrected version of the Oppenheimer--Snyder (OS) spacetime in which classical collapse is modified by a single effective-parameter α, representing small-quantum-gravitational effects in a phenomenologically rescaled-form. Although the correction enters through a term proportional to αM2/r4, it produces noticeable changes in the strong-field region while leaving weak-field physics almost unchanged. One of the main results is the appearance of a minimum-mass for horizon-formation, Mmin ∼(0.5−1.2) M⊙ for the effective-parameter α≈0.22. We emphasize that this Mmin is expressed in terms of the effective-parameter α; in terms of the bare loop-quantum-gravity (LQG) parameter, Mmin∼ MPl∼10−5~g, consistent with the theoretical-expectation. Orbital properties are also slightly modified, with the innermost-stable-circular-orbit (ISCO) shifting to rISCO=6M−α/(12M), giving corrections-of-order ∼ 10−4 for stellar-black-holes and ∼ 10−10 for Sgr A∗. In the same region, radial epicyclic frequencies change by about 5%−10% near r∼5M, while vertical modes are less affected, leading to small but structured shifts in quasi-periodic oscillation (QPO) behavior. Using four X-ray binaries (GRS 1915+105, XTE J1550-564, XTE J1859+226, GRO J1655-40), we find a consistent range α=0.22±0.10, with masses between 5.4−12.4 M⊙ and emission radii r/M ∼ 5.5 − 8.6. The observed QPO frequencies, lying in the range 100−450 Hz, are well reproduced within this framework. Weak-field tests such as S2 and Mercury still allow fsp=1.10 ± 0.19, leaving room for these small strong-gravity corrections.
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BibTeX
@misc{errehymy2026joint,
title = {{Joint Constraints on Quantum Oppenheimer--Snyder Black Holes from High-Frequency Quasi-Periodic Oscillations in X-ray Binary Systems and the S2 Star Orbit}},
author = {A. Errehymy and Y. Khedif and M. Daoud and B. Turimov and S. Usanov and F. Turaev and Z. Yasakov},
howpublished = {arXiv},
year = {2026},
month = sep,
doi = {10.48550/arxiv.2609.16018},
eprint = {2609.16018},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2609.16018},
}
RIS
TY - UNPB
TI - Joint Constraints on Quantum Oppenheimer--Snyder Black Holes from High-Frequency Quasi-Periodic Oscillations in X-ray Binary Systems and the S2 Star Orbit
AU - A. Errehymy
AU - Y. Khedif
AU - M. Daoud
AU - B. Turimov
AU - S. Usanov
AU - F. Turaev
AU - Z. Yasakov
PY - 2026
DA - 2026/09/05
PB - arXiv
DO - 10.48550/arxiv.2609.16018
UR - https://arxiv.org/abs/2609.16018
AB - We study a quantum-corrected version of the Oppenheimer--Snyder (OS) spacetime in which classical collapse is modified by a single effective-parameter α, representing small-quantum-gravitational effects in a phenomenologically rescaled-form. Although the correction enters through a term proportional to αM^2/r^4, it produces noticeable changes in the strong-field region while leaving weak-field physics almost unchanged. One of the main results is the appearance of a minimum-mass for horizon-formation, M_min ∼(0.5−1.2) M_⊙ for the effective-parameter α≈0.22. We emphasize that this M_min is expressed in terms of the effective-parameter α; in terms of the bare loop-quantum-gravity (LQG) parameter, M_min∼ M_Pl∼10^−5~g, consistent with the theoretical-expectation. Orbital properties are also slightly modified, with the innermost-stable-circular-orbit (ISCO) shifting to r_ISCO=6M−α/(12M), giving corrections-of-order ∼ 10^−4 for stellar-black-holes and ∼ 10^−10 for Sgr A^∗. In the same region, radial epicyclic frequencies change by about 5%−10% near r∼5M, while vertical modes are less affected, leading to small but structured shifts in quasi-periodic oscillation (QPO) behavior. Using four X-ray binaries (GRS 1915+105, XTE J1550-564, XTE J1859+226, GRO J1655-40), we find a consistent range α=0.22±0.10, with masses between 5.4−12.4 M_⊙ and emission radii r/M ∼ 5.5 − 8.6. The observed QPO frequencies, lying in the range 100−450 Hz, are well reproduced within this framework. Weak-field tests such as S2 and Mercury still allow f_sp=1.10 ± 0.19, leaving room for these small strong-gravity corrections.
ER -