Shadow signatures and near-horizon energy accumulation in coherent quantum sine-integral black holes
Abstract
Quantum modifications of black hole spacetimes can lead to observable departures from the predictions of classical general relativity, particularly in the strong-gravity regime near the event horizon. In this context, the coherent quantum black hole model introduces a sine-integral correction to the gravitational potential, characterized by a coherence scale Rs, which softens the central singularity and alters the near-horizon geometry. Motivated by the growing precision of black hole imaging and strong-field observations, we explore how these quantum-induced effects influence photon motion and the resulting shadow structure. Considering representative values within the interval Rs ∈ [0.5M, 1.2M], we show that the photon sphere shifts inward while the critical impact parameter decreases, reaching values such as bcrit≈ 4.764M for Rs=0.5M. Consequently, the shadow radius becomes systematically smaller and develops a more intricate structure than in the Schwarzschild case (bcrit=3√3M ≈ 5.196M). The analysis of the corresponding intensity distributions also reveals a pronounced enhancement of radiation near the shadow boundary, especially for intermediate coherence scales. This feature can be attributed to photons remaining longer within the modified near-horizon region before escaping toward distant observers. Such an increase in brightness may therefore provide a possible observational signature of quantum corrections at horizon scales. Furthermore, although the geometry allows radiation and energy to accumulate around an effective horizon surface, its response to perturbations differs from that expected for compact objects with stable light rings. Instead of contracting under backreaction effects, the accumulation surface shifts outward.
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BibTeX
@misc{errehymy2026shadow,
title = {{Shadow signatures and near-horizon energy accumulation in coherent quantum sine-integral black holes}},
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.2610.08841},
eprint = {2610.08841},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2610.08841},
}
RIS
TY - UNPB
TI - Shadow signatures and near-horizon energy accumulation in coherent quantum sine-integral black holes
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.2610.08841
UR - https://arxiv.org/abs/2610.08841
AB - Quantum modifications of black hole spacetimes can lead to observable departures from the predictions of classical general relativity, particularly in the strong-gravity regime near the event horizon. In this context, the coherent quantum black hole model introduces a sine-integral correction to the gravitational potential, characterized by a coherence scale R_s, which softens the central singularity and alters the near-horizon geometry. Motivated by the growing precision of black hole imaging and strong-field observations, we explore how these quantum-induced effects influence photon motion and the resulting shadow structure. Considering representative values within the interval R_s ∈ [0.5M, 1.2M], we show that the photon sphere shifts inward while the critical impact parameter decreases, reaching values such as b_crit≈ 4.764M for R_s=0.5M. Consequently, the shadow radius becomes systematically smaller and develops a more intricate structure than in the Schwarzschild case (b_crit=3√3M ≈ 5.196M). The analysis of the corresponding intensity distributions also reveals a pronounced enhancement of radiation near the shadow boundary, especially for intermediate coherence scales. This feature can be attributed to photons remaining longer within the modified near-horizon region before escaping toward distant observers. Such an increase in brightness may therefore provide a possible observational signature of quantum corrections at horizon scales. Furthermore, although the geometry allows radiation and energy to accumulate around an effective horizon surface, its response to perturbations differs from that expected for compact objects with stable light rings. Instead of contracting under backreaction effects, the accumulation surface shifts outward.
ER -