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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Skvortsova, Fortsch
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abstract
While $(2+1)$-dimensional black holes in the Einstein theory allow for only the anti-de Sitter asymptotic, when the higher curvature correction is tuned on, the asymptotically flat, de Sitter and anti-de Sitter cases are included. Here we propose first comprehensive study of the stability and quasinormal spectra of the scalar field perturbations around such black holes with all three asymptotics. Calculations of the frequencies are fulfilled with the help of the 6th order WKB method with Pade approximants, Bernstein polynomial method and time-domain integration. Results obtained by all three methods are in a very good agreement in their common range of applicability. When the multipole moment $k$ is equal to zero, the purely imaginary, i.e. non-oscillatory, modes dominate in the spectrum for all types of the asymptotic behavior, while the spectrum at higher $k$ resembles that in four-dimensional spacetime with the corresponding asymptotic.
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gr-qc 16years
2026 16roles
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Scattering and Hawking Radiation from Einstein--Euler--Heisenberg--de Sitter Black Holes
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Greybody Factors, Absorption Cross Sections and Hawking Radiation of Holonomy-Corrected Schwarzschild Black Holes
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Grey-Body Factors and Thermodynamics of Asymptotically de Sitter Black Holes in Generalized Proca Theory
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Long-lived quasinormal modes of Asymptotically de Sitter Black Holes in Generalized Proca Theory
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Massive scalar quasinormal modes of an asymptotically flat regular black hole supported by a phantom Dirac--Born--Infeld field
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