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.
Late time tails of the massive vector field in a black hole background
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abstract
We investigate the late-time behavior of the massive vector field in the background of the Schwarzschild and Schwarzschild-de Sitter black holes. For Schwarzschild black hole, at intermediately late times the massive vector field is represented by three functions with different decay law $\Psi_{0} \sim t^{-(\ell + 3/2)} \sin{m t}$, $\Psi_{1} \sim t^{-(\ell + 5/2)} \sin{m t}$, $\Psi_{2} \sim t^{-(\ell + 1/2)} \sin{m t}$, while at asymptotically late times the decay law $\Psi \sim t^{-5/6} \sin{(m t)}$ is universal, and does not depend on the multipole number $\ell$. Together with previous study of massive scalar and Dirac fields where the same asymptotically late-time decay law was found, it means, that the asymptotically late-time decay law $\sim t^{-5/6} \sin{(m t)}$ \emph{does not depend} also \emph{on the spin} of the field under consideration. For Schwarzschild-de Sitter black holes it is observed two different regimes in the late-time decay of perturbations: non-oscillatory exponential damping for small values of $m$ and oscillatory quasinormal mode decay for high enough $m$. Numerical and analytical results are found for these quasinormal frequencies.
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Massive scalar perturbations of de Sitter black holes in generalized Proca theory enter a large-mass regime with linearly growing real frequencies and constant damping rates, without true quasi-resonances, plus an analytic formula and shifts due to black-hole size and Proca hair.
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.
First-order eikonal formulas connect a scalarized black-hole metric to quasinormal modes, shadows, strong lensing, and grey-body factors via photon-sphere invariants in the weak-hair limit.
This review surveys calculations and interpretations of quasinormal modes for black holes in astrophysics, higher dimensions, and holographic duals without presenting new results.
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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Long-lived quasinormal modes of Asymptotically de Sitter Black Holes in Generalized Proca Theory
Massive scalar perturbations of de Sitter black holes in generalized Proca theory enter a large-mass regime with linearly growing real frequencies and constant damping rates, without true quasi-resonances, plus an analytic formula and shifts due to black-hole size and Proca hair.
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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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A First-Order Eikonal Framework for Quasinormal Modes, Shadows, Strong Lensing, and Grey-Body Factors in a Scalarized Black-Hole Metric
First-order eikonal formulas connect a scalarized black-hole metric to quasinormal modes, shadows, strong lensing, and grey-body factors via photon-sphere invariants in the weak-hair limit.
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Quasinormal modes of black holes: from astrophysics to string theory
This review surveys calculations and interpretations of quasinormal modes for black holes in astrophysics, higher dimensions, and holographic duals without presenting new results.