In asymmetric Damour-Solodukhin wormholes, reflectionless and echo modes share asymptotic spectral properties parallel to the real frequency axis with matching spacing, and reflectionless modes lie closer to the axis yielding larger echo amplitudes.
Quantifying excita tions of quasinormal mode systems
5 Pith papers cite this work. Polarity classification is still indexing.
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abstract
Computations of the strong field generation of gravitational waves by black hole processes produce waveforms that are dominated by quasinormal (QN) ringing, a damped oscillation characteristic of the black hole. We describe here the mathematical problem of quantifying the QN content of the waveforms generated. This is done in several steps: (i) We develop the mathematics of QN systems that are complete (in a sense to be defined) and show that there is a quantity, the ``excitation coefficient,'' that appears to have the properties needed to quantify QN content. (ii) We show that incomplete systems can (at least sometimes) be converted to physically equivalent complete systems. Most notably, we give a rigorous proof of completeness for a specific modified model problem. (iii) We evaluate the excitation coefficient for the model problem, and demonstrate that the excitation coefficient is of limited utility. We finish by discussing the general question of quantification of QN excitations, and offer a few speculations about unavoidable differences between normal mode and QN systems.
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Black hole fundamental quasinormal modes exhibit strong sensitivity to small perturbations in the effective potential, with the instability type depending on the potential shape and perturbation distance from the black hole.
Simulation-based inference reliably extracts physical parameters from noisy spectra of analogue black holes.
Quasinormal modes are eigenmodes of dissipative gravitational systems whose spectra encode near-equilibrium transport coefficients in dual quantum field theories and enable tests of general relativity through gravitational wave observations.
A review summarizing the properties, calculation methods, and astrophysical relevance of quasi-normal modes for Schwarzschild, Reissner-Nordström, Kerr, Kerr-Newman black holes and non-rotating or slowly-rotating stars.
citing papers explorer
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Reflectionless and echo modes in asymmetric Damour-Solodukhin wormholes
In asymmetric Damour-Solodukhin wormholes, reflectionless and echo modes share asymptotic spectral properties parallel to the real frequency axis with matching spacing, and reflectionless modes lie closer to the axis yielding larger echo amplitudes.
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Sensitivity of black hole spectral instability against perturbations of the effective potential
Black hole fundamental quasinormal modes exhibit strong sensitivity to small perturbations in the effective potential, with the instability type depending on the potential shape and perturbation distance from the black hole.
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Spectroscopy of analogue black holes using simulation-based inference
Simulation-based inference reliably extracts physical parameters from noisy spectra of analogue black holes.
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Quasinormal modes of black holes and black branes
Quasinormal modes are eigenmodes of dissipative gravitational systems whose spectra encode near-equilibrium transport coefficients in dual quantum field theories and enable tests of general relativity through gravitational wave observations.
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Quasi-Normal Modes of Stars and Black Holes
A review summarizing the properties, calculation methods, and astrophysical relevance of quasi-normal modes for Schwarzschild, Reissner-Nordström, Kerr, Kerr-Newman black holes and non-rotating or slowly-rotating stars.