Greybody Factors and Hawking Spectra of Quantum-Corrected Black Holes
Abstract
We investigate Hawking radiation of a quantum-corrected Schwarzschild black hole with vacuum polarization and conformal anomaly effects. The corrected geometry has two horizons, a non-monotonic Hawking temperature that vanishes at a critical mass, and a logarithmic entropy correction. We compute greybody factors, spectra, and emission rates for massless bosonic fields of various spins and angular momenta. Quantum corrections suppress low-energy greybody factors and enhance high-energy ones. During late evaporation, where quantum influences become significant, the decreasing temperature strongly suppresses emission. In this case, the higher-spin modes become negligible, and the scalar s=l=0 mode dominates. The black hole lifetime is greatly extended as it asymptotically approaches a stable extremal remnant.
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BibTeX
@misc{shafiee2026greybody,
title = {{Greybody Factors and Hawking Spectra of Quantum-Corrected Black Holes}},
author = {Moslem Shafiee and Ahmad Sheykhi},
howpublished = {arXiv},
year = {2026},
month = sep,
doi = {10.48550/arxiv.2609.32702},
eprint = {2609.32702},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2609.32702},
}
RIS
TY - UNPB
TI - Greybody Factors and Hawking Spectra of Quantum-Corrected Black Holes
AU - Moslem Shafiee
AU - Ahmad Sheykhi
PY - 2026
DA - 2026/09/26
PB - arXiv
DO - 10.48550/arxiv.2609.32702
UR - https://arxiv.org/abs/2609.32702
AB - We investigate Hawking radiation of a quantum-corrected Schwarzschild black hole with vacuum polarization and conformal anomaly effects. The corrected geometry has two horizons, a non-monotonic Hawking temperature that vanishes at a critical mass, and a logarithmic entropy correction. We compute greybody factors, spectra, and emission rates for massless bosonic fields of various spins and angular momenta. Quantum corrections suppress low-energy greybody factors and enhance high-energy ones. During late evaporation, where quantum influences become significant, the decreasing temperature strongly suppresses emission. In this case, the higher-spin modes become negligible, and the scalar s=l=0 mode dominates. The black hole lifetime is greatly extended as it asymptotically approaches a stable extremal remnant.
ER -