Accretion dynamics of thin and thick disks in charged Kalb-Ramond black holes
Abstract
In this work, we investigate the accretion properties of an electrically charged, static, spherically symmetric black hole in Kalb-Ramond (KR) gravity, where a dimensionless parameter l characterizes spontaneous Lorentz symmetry-breaking. We first constrain the free charge and KR parameter space, (Q,l), by comparing the predicted shadow radius of this family of solutions with the bounds inferred from Event Horizon Telescope observations of Sagittarius A*. The inclusion of electric charge introduces a degeneracy between Q and l, enlarging the region compatible with the observed shadow size and yielding the broad constraint −0.3900 ≤ l ≤ 0.1898, with part of the compatible parameter space extending into the naked-singularity sector. We then investigate relativistic accretion disks around the charged KR black hole within the above constraints. For geometrically thin disks, we compute the time averaged energy flux, temperature distribution, emission spectrum, time averaged torque, and mass-to-radiation conversion efficiency, finding that the radiative output increases for higher values of l, while lower values of l suppress it. Furthermore, when coupled with the electric charge this effect is amplified. For geometrically thick, constant-angular momentum tori-shaped disks, Lorentz symmetry-breaking shifts the characteristic orbital radii, compresses the radial extent of equilibrium configurations, narrows the interval supporting finite equilibrium tori, and shifts the stationary-fluid topology toward open and unconfined configurations outside that interval. These results show how charge and spontaneous Lorentz symmetry-breaking jointly affect observational constraints and the structure and emission properties of black hole accretion flows, providing potential signatures of KR gravity in the strong-gravity regime.
Related
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BibTeX
@misc{junior2026accretion,
title = {{Accretion dynamics of thin and thick disks in charged Kalb-Ramond black holes}},
author = {Ednaldo L. B. Junior and José Tarciso S. S. Junior and Francisco S. N. Lobo and Jorde A. A. Ramos and Manuel E. Rodrigues and Diego Rubiera-Garcia and Luís F. Dias da Silva and Henrique A. Vieira},
howpublished = {arXiv},
year = {2026},
month = sep,
doi = {10.48550/arxiv.2609.02223},
eprint = {2609.02223},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2609.02223},
note = {CC BY 4.0},
}
RIS
TY - UNPB
TI - Accretion dynamics of thin and thick disks in charged Kalb-Ramond black holes
AU - Ednaldo L. B. Junior
AU - José Tarciso S. S. Junior
AU - Francisco S. N. Lobo
AU - Jorde A. A. Ramos
AU - Manuel E. Rodrigues
AU - Diego Rubiera-Garcia
AU - Luís F. Dias da Silva
AU - Henrique A. Vieira
PY - 2026
DA - 2026/09/02
PB - arXiv
DO - 10.48550/arxiv.2609.02223
UR - https://arxiv.org/abs/2609.02223
AB - In this work, we investigate the accretion properties of an electrically charged, static, spherically symmetric black hole in Kalb-Ramond (KR) gravity, where a dimensionless parameter l characterizes spontaneous Lorentz symmetry-breaking. We first constrain the free charge and KR parameter space, (Q,l), by comparing the predicted shadow radius of this family of solutions with the bounds inferred from Event Horizon Telescope observations of Sagittarius A*. The inclusion of electric charge introduces a degeneracy between Q and l, enlarging the region compatible with the observed shadow size and yielding the broad constraint −0.3900 ≤ l ≤ 0.1898, with part of the compatible parameter space extending into the naked-singularity sector. We then investigate relativistic accretion disks around the charged KR black hole within the above constraints. For geometrically thin disks, we compute the time averaged energy flux, temperature distribution, emission spectrum, time averaged torque, and mass-to-radiation conversion efficiency, finding that the radiative output increases for higher values of l, while lower values of l suppress it. Furthermore, when coupled with the electric charge this effect is amplified. For geometrically thick, constant-angular momentum tori-shaped disks, Lorentz symmetry-breaking shifts the characteristic orbital radii, compresses the radial extent of equilibrium configurations, narrows the interval supporting finite equilibrium tori, and shifts the stationary-fluid topology toward open and unconfined configurations outside that interval. These results show how charge and spontaneous Lorentz symmetry-breaking jointly affect observational constraints and the structure and emission properties of black hole accretion flows, providing potential signatures of KR gravity in the strong-gravity regime.
ER -