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A Matrix Method for Quasinormal Modes: Kerr and Kerr-Sen Black Holes

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arxiv 1703.06439 v2 pith:HAIWTUET submitted 2017-03-19 gr-qc

Kai Lin , Wei-Liang Qian , Alan B. Pavan , Elcio Abdalla This is my paper · ORCID
classification gr-qc
keywords matrixmethodquasinormalmodesangularblackequationholes
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abstract

In this letter, a matrix method is employed to study the scalar quasinormal modes of Kerr as well as Kerr-Sen black holes. Discretization is applied to transfer the scalar perturbation equation into a matrix form eigenvalue problem, where the resulting radial and angular equations are derived by the method of separation of variables. The eigenvalues, quasinormal frequencies $\omega$ and angular quantum numbers $\lambda$, are then obtained by numerically solving the resultant homogeneous matrix equation. This work shows that the present approach is an accurate as well as efficient method for investigating quasinormal modes.

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Cited by 2 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Late-Time Cosmology and Structure Formation in Quadratic $f(Q)$ Gravity

    physics.gen-ph 2026-06 unverdicted novelty 4.0 of 10

    Quadratic f(Q) gravity adds an H^4 term to the Friedmann equation and introduces a time-dependent G_eff that suppresses linear growth and halo abundance, offering a modified-gravity route to easing the S8 tension.

  2. Quasinormal Modes and Dynamical Evolution of Scalar Fields in the Einstein-Bumblebee Theory with a Cosmological Constant

    gr-qc 2025-02 conditional novelty 4.0 of 10

    For scalar perturbations of Einstein-Bumblebee black holes in de Sitter spacetime, increasing the Lorentz-violation parameter or the cosmological constant generally lowers the quasinormal mode frequency and damping rate.

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