https://doi.org/10.1140/epjc/s10052-025-14996-z
Regular Article - Theoretical Physics
Quasinormal modes and greybody factors of charged symmergent black hole
1
Department of Physics, Moran College, Moranhat, 785670, Charaideo, Assam, India
2
Research Center of Astrophysics and Cosmology, Khazar University, 41 Mehseti Street, AZ1096, Baku, Azerbaijan
3
Faculty of Engineering and Natural Sciences, Sabancı University, 34956, Tuzla, İstanbul, Turkey
4
Astrophysics Research Center (ARCO), The Open University of Israel, 4353701, Raanana, Israel
5
Physics Department, Eastern Mediterranean University, North Cyprus via Mersin 10, 99628, Famagusta, Turkey
a
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Received:
27
December
2024
Accepted:
26
October
2025
Published online:
3
November
2025
In this paper, we investigate quasinormal modes (QNMs) and greybody factors within the framework of Symmergent gravity, an emergent gravity model with an 
curvature sector. Building on our previous work on static spherically-symmetric solutions [Puliçe et al. in Class Quantum Gravity 40(19):195003, 2023], we explore the effects of the key parameters, including the quadratic curvature coupling parameter 
and the vacuum energy parameter 
. For all the three perturbations considered here viz., scalar, electromagnetic and gravitational perturbations, an increase in leads to a nearly linear rise in both oscillation frequencies and damping rates. The other parameter affects the QNMs spectrum nonlinearly. Additionally, the charge Q of the black hole introduces nonlinear behavior, where higher charges amplify the black hole’s electromagnetic field, resulting in increased oscillation frequencies and faster stabilization. These findings enhance our understanding of charged black hole stability and gravitational wave astrophysics. Further, the analysis of greybody factors reveals that increasing , , and Q reduces the absorption of radiation, with gravitational perturbations reaching maximum absorption at slightly lower frequencies compared to electromagnetic and scalar perturbations.
© The Author(s) 2025
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