Gravitational Waves from Ringing Dyonic Black Holes and Estimation of Parameters in Einstein-Bumblebee-Maxwell Gravity
Abstract
In this work, we investigate the quasinormal mode (QNM) frequencies of dyonic Reissner-Nordström (RN)-like black holes associated with scalar and gravitational perturbations in the framework of Einstein-bumblebee-Maxwell gravity theory. The QNMs are calculated using the 6th-order Padé averaged WKB approximation method. We analyse the dependence of oscillation frequencies and damping rate of the BHs for the free model parameters. To further verify the QNM spectrum, we study the time evolution of both the scalar and gravitational perturbations around the BHs and extract the dominant QNM from the resulting ringdown signal. Moreover, we try to estimate the BH parameters using Fisher analysis method for the future gravitational wave detector named Laser Interferometer Space Antenna (LISA). We found that for supermassive BHs with mass around 106 -- 108 M⊙ and at lower redshifts, the signal-to-noise ratio for the detection of a QNM signal by the LISA is high. Further, for a representative source at a luminosity distance of $3$ Gpc, the BH mass at the detector reference frame and the Lorentz violating parameter are well constrained for supermassive BHs with mass ≥ 106.
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BibTeX
@misc{gogoi2026gravitational,
title = {{Gravitational Waves from Ringing Dyonic Black Holes and Estimation of Parameters in Einstein-Bumblebee-Maxwell Gravity}},
author = {Sikha Gogoi and Umananda Dev Goswami},
howpublished = {arXiv},
year = {2026},
month = oct,
doi = {10.48550/arxiv.2610.33569},
eprint = {2610.33569},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2610.33569},
note = {CC BY 4.0},
}
RIS
TY - UNPB
TI - Gravitational Waves from Ringing Dyonic Black Holes and Estimation of Parameters in Einstein-Bumblebee-Maxwell Gravity
AU - Sikha Gogoi
AU - Umananda Dev Goswami
PY - 2026
DA - 2026/10/24
PB - arXiv
DO - 10.48550/arxiv.2610.33569
UR - https://arxiv.org/abs/2610.33569
AB - In this work, we investigate the quasinormal mode (QNM) frequencies of dyonic Reissner-Nordström (RN)-like black holes associated with scalar and gravitational perturbations in the framework of Einstein-bumblebee-Maxwell gravity theory. The QNMs are calculated using the 6th-order Padé averaged WKB approximation method. We analyse the dependence of oscillation frequencies and damping rate of the BHs for the free model parameters. To further verify the QNM spectrum, we study the time evolution of both the scalar and gravitational perturbations around the BHs and extract the dominant QNM from the resulting ringdown signal. Moreover, we try to estimate the BH parameters using Fisher analysis method for the future gravitational wave detector named Laser Interferometer Space Antenna (LISA). We found that for supermassive BHs with mass around 10^6 -- 10^8 M_⊙ and at lower redshifts, the signal-to-noise ratio for the detection of a QNM signal by the LISA is high. Further, for a representative source at a luminosity distance of $3$ Gpc, the BH mass at the detector reference frame and the Lorentz violating parameter are well constrained for supermassive BHs with mass ≥ 10^6.
ER -