Polarization Transport and Polarized Images of a Rotating Braneworld Black Hole
Abstract
We investigate polarized synchrotron emission from an optically thin accretion flow around a rotating braneworld black hole, focusing on how higher-dimensional gravity modifies photon propagation and polarization transport. We integrate the null-geodesic and parallel-transport equations for the polarization four-vector and, within a common emissivity and magnetic-field prescription, examine the effects of tidal charge, black-hole spin, observer inclination, and prograde or retrograde orbital motion. We analyze the linearly polarized intensity, electric-vector position angle (EVPA), Stokes parameters, the joint Q--U polarization-state space, and the cumulative net linear polarization degree, and compare representative braneworld configurations with Kerr and Kerr--Newman spacetimes. Within the parameter range considered, tidal charge and spin do not generate a qualitatively new large-scale polarization morphology. Instead, they primarily reorganize the polarized intensity, orientation, and polarization-state distribution in the strong-field region near the shadow boundary and photon ring. Viewing inclination controls the dominant projected morphology, while high inclinations enhance projection and Doppler asymmetries and make the distinction between prograde and retrograde flows more pronounced. The Stokes components and their joint state space expose local bending, stretching, and trajectory concentration that are less apparent in intensity images. The cumulative net linear polarization degree decreases with increasing cumulative radius, and larger tidal charge or spin lowers its amplitude for the representative models considered. Together, these complementary polarization observables provide a potential route for separating spacetime, viewing-geometry, and accretion-flow effects and for constraining braneworld tidal charge with horizon-scale polarimetry.
Related
- Horizon-scale intensity and polarization images of rotating Konoplya-Zhidenko black holes with thick accretion flows
- Optical Images of the Braneworld Black Hole Surrounded by an Optically Thin Accretion Disk
- Shadow and Polarized Images of Schwarzschild-MOG Black Hole Illuminated by Thick Accretion Disk
- Formation dynamics of a rotating solar spicule-like event and associated energy-mass transport
- Model of the instrumental polarization induced by a rotating HWP with anti-reflective sub-wavelength structures for CMB polarimetry
BibTeX
@misc{deng2026polarization,
title = {{Polarization Transport and Polarized Images of a Rotating Braneworld Black Hole}},
author = {Wen-Hao Deng and Qing-Quan Jiang and Kai Lin and Pei Wang},
howpublished = {arXiv},
year = {2026},
month = oct,
doi = {10.48550/arxiv.2610.03738},
eprint = {2610.03738},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2610.03738},
}
RIS
TY - UNPB
TI - Polarization Transport and Polarized Images of a Rotating Braneworld Black Hole
AU - Wen-Hao Deng
AU - Qing-Quan Jiang
AU - Kai Lin
AU - Pei Wang
PY - 2026
DA - 2026/10/01
PB - arXiv
DO - 10.48550/arxiv.2610.03738
UR - https://arxiv.org/abs/2610.03738
AB - We investigate polarized synchrotron emission from an optically thin accretion flow around a rotating braneworld black hole, focusing on how higher-dimensional gravity modifies photon propagation and polarization transport. We integrate the null-geodesic and parallel-transport equations for the polarization four-vector and, within a common emissivity and magnetic-field prescription, examine the effects of tidal charge, black-hole spin, observer inclination, and prograde or retrograde orbital motion. We analyze the linearly polarized intensity, electric-vector position angle (EVPA), Stokes parameters, the joint Q--U polarization-state space, and the cumulative net linear polarization degree, and compare representative braneworld configurations with Kerr and Kerr--Newman spacetimes. Within the parameter range considered, tidal charge and spin do not generate a qualitatively new large-scale polarization morphology. Instead, they primarily reorganize the polarized intensity, orientation, and polarization-state distribution in the strong-field region near the shadow boundary and photon ring. Viewing inclination controls the dominant projected morphology, while high inclinations enhance projection and Doppler asymmetries and make the distinction between prograde and retrograde flows more pronounced. The Stokes components and their joint state space expose local bending, stretching, and trajectory concentration that are less apparent in intensity images. The cumulative net linear polarization degree decreases with increasing cumulative radius, and larger tidal charge or spin lowers its amplitude for the representative models considered. Together, these complementary polarization observables provide a potential route for separating spacetime, viewing-geometry, and accretion-flow effects and for constraining braneworld tidal charge with horizon-scale polarimetry.
ER -