Quasinormal modes of massive scalars in CFM brane-world black holes split into two types, with modes disappearing at critical masses where real or imaginary frequency parts reach zero.
Mixed citations
Decay of massive scalar field in a black hole background immersed in magnetic field
Mixed citation behavior. Most common role is background (67%).
7
Pith papers citing it
Background
67% of classified citations
abstract
We evaluate quasinormal modes of massive scalar field of the Ernst spacetime, an exact solution of the Einstein-Maxwell equations describing a black hole immersed in uniform magnetic field $B$. It is known that the quasinormal spectrum for massive scalar field in the vicinity of the magnetized black holes acquires an effective mass $\mu_{eff}= \sqrt{4B^2 m^2+\mu^2}$, where $m$ is the azimuthal number and $\mu$ is the mass of scalar field. The numerical result shows that increasing of the field effective mass and the magnetic field $B$ gives rise to decreasing of the imaginary part of the quasinormal modes until reaching the vanishing damping rate.
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gr-qc 7years
2026 7verdicts
UNVERDICTED 7roles
background 6representative citing papers
Increasing the mass of a scalar field around a parity-symmetric beyond-Horndeski black hole strongly reduces the damping rate of quasinormal modes while suppressing low-frequency absorption and shifting efficient absorption to higher frequencies.
Massive scalar quasinormal modes in quasi-topological black holes become long-lived as scalar mass grows, while photon-sphere radius, shadow size, and ISCO exhibit moderate deviations from Schwarzschild.
Positive tidal charge in this brane-world black hole lowers the effective potential barrier, pushes massive scalar quasinormal modes toward arbitrarily long lifetimes, and increases transmission and absorption.
Increasing the mass of a perturbing scalar field around Einstein-Maxwell-dilaton black holes strongly suppresses damping in several quasinormal branches, producing quasi-resonant long-lived oscillations.
Massive scalar perturbations on the Dymnikova regular black hole exhibit growing oscillation frequencies, reduced damping rates leading to quasi-resonances, power-law oscillatory tails, and mass-dependent suppression of grey-body factors.
Massive scalar quasinormal modes in this DBI-supported regular black hole show higher oscillation frequencies and lower damping as field mass increases, with larger regularity scales producing softer and longer-lived ringing.
citing papers explorer
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Two types of quasinormal modes of Casadio-Fabbri-Mazzacurati brane-world black holes
Quasinormal modes of massive scalars in CFM brane-world black holes split into two types, with modes disappearing at critical masses where real or imaginary frequency parts reach zero.
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Massive Scalar Quasinormal Modes, Greybody Factors, and Absorption Cross Section of a Parity-Symmetric Beyond-Horndeski Black Hole
Increasing the mass of a scalar field around a parity-symmetric beyond-Horndeski black hole strongly reduces the damping rate of quasinormal modes while suppressing low-frequency absorption and shifting efficient absorption to higher frequencies.
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Long-lived quasinormal modes, shadows and particle motion in four-dimensional quasi-topological gravity
Massive scalar quasinormal modes in quasi-topological black holes become long-lived as scalar mass grows, while photon-sphere radius, shadow size, and ISCO exhibit moderate deviations from Schwarzschild.
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Long-lived massive scalar modes, grey-body factors, and absorption cross sections of the Reissner--Nordstr\"om-like brane-world black hole
Positive tidal charge in this brane-world black hole lowers the effective potential barrier, pushes massive scalar quasinormal modes toward arbitrarily long lifetimes, and increases transmission and absorption.
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Quasi-resonances in the vicinity of Einstein-Maxwell-dilaton black hole
Increasing the mass of a perturbing scalar field around Einstein-Maxwell-dilaton black holes strongly suppresses damping in several quasinormal branches, producing quasi-resonant long-lived oscillations.
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Telling tails and quasi-resonances in the vicinity of Dymnikova regular black hole
Massive scalar perturbations on the Dymnikova regular black hole exhibit growing oscillation frequencies, reduced damping rates leading to quasi-resonances, power-law oscillatory tails, and mass-dependent suppression of grey-body factors.
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Massive scalar quasinormal modes of an asymptotically flat regular black hole supported by a phantom Dirac--Born--Infeld field
Massive scalar quasinormal modes in this DBI-supported regular black hole show higher oscillation frequencies and lower damping as field mass increases, with larger regularity scales producing softer and longer-lived ringing.