Scalar, vector, and tensor perturbations on the Kerr spacetime are governed by equations that can be solved by separation of variables, but the same is not true in generic stationary and axisymmetric geometries. This complicates the calculation of black-hole quasinormal mode frequencies in theories that extend/modify general relativity, because one generally has to calculate the eigenvalue spectrum of a two-dimensional partial differential equation (in the radial and angular variables) instead of an ordinary differential equation (in the radial variable). In this work, we show that if the background geometry is close to the Kerr one, the problem considerably simplifies. One can indeed compute the quasinormal mode frequencies, at least at leading order in the deviation from Kerr, by solving an ordinary differential equation subject to suitable boundary conditions. Although our method is general, in this paper we apply it to scalar perturbations on top of a Kerr black hole with an anomalous quadrupole moment, or on top of a slowly rotating Kerr background.

Quasinormal modes of nonseparable perturbation equations: The scalar non-Kerr case / Ghosh, Rajes; Franchini, Nicola; Völkel, Sebastian H.; Barausse, Enrico. - In: PHYSICAL REVIEW D. - ISSN 2470-0010. - 108:2(2023), pp. 1-13. [10.1103/PhysRevD.108.024038]

Quasinormal modes of nonseparable perturbation equations: The scalar non-Kerr case

Franchini, Nicola;Barausse, Enrico
2023-01-01

Abstract

Scalar, vector, and tensor perturbations on the Kerr spacetime are governed by equations that can be solved by separation of variables, but the same is not true in generic stationary and axisymmetric geometries. This complicates the calculation of black-hole quasinormal mode frequencies in theories that extend/modify general relativity, because one generally has to calculate the eigenvalue spectrum of a two-dimensional partial differential equation (in the radial and angular variables) instead of an ordinary differential equation (in the radial variable). In this work, we show that if the background geometry is close to the Kerr one, the problem considerably simplifies. One can indeed compute the quasinormal mode frequencies, at least at leading order in the deviation from Kerr, by solving an ordinary differential equation subject to suitable boundary conditions. Although our method is general, in this paper we apply it to scalar perturbations on top of a Kerr black hole with an anomalous quadrupole moment, or on top of a slowly rotating Kerr background.
2023
108
2
1
13
024038
10.1103/PhysRevD.108.024038
https://arxiv.org/abs/2303.00088
Ghosh, Rajes; Franchini, Nicola; Völkel, Sebastian H.; Barausse, Enrico
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/20.500.11767/133030
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