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Gravitational perturbations and quasinormal modes of Black holes with non-spherical topology. (English) Zbl 1117.83069

Summary: We investigate the physical interpretation of gravitational perturbations of static asymptotically anti-de Sitter black holes with non-spherical topology. For zero wavenumber modes, the axial perturbations yield only small rotations on the system, while the polar perturbations lead to a change in the mass and may also produce gravitational waves. Additionally, it is verified that perturbations with any nonzero wavenumber are able to produce gravitational waves in these space-times. On the basis of these results, the quasinormal frequencies corresponding to polar perturbation modes with null wavenumber are calculated and briefly analyzed.

MSC:

83C57 Black holes
83C25 Approximation procedures, weak fields in general relativity and gravitational theory
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References:

[1] Misner C. W., Gravitation (1973)
[2] DOI: 10.7208/chicago/9780226870373.001.0001 · Zbl 0549.53001 · doi:10.7208/chicago/9780226870373.001.0001
[3] DOI: 10.1016/0375-9601(95)00229-V · Zbl 1020.83608 · doi:10.1016/0375-9601(95)00229-V
[4] DOI: 10.1016/0370-2693(95)00533-Q · doi:10.1016/0370-2693(95)00533-Q
[5] DOI: 10.1103/PhysRevD.54.4891 · doi:10.1103/PhysRevD.54.4891
[6] Chandrasekhar S., The Mathematical Theory of Black Holes (1983) · Zbl 0511.53076
[7] Kokkotas K. D., Living Rev. Rel. 2 pp 2–
[8] DOI: 10.1103/PhysRevD.62.024027 · doi:10.1103/PhysRevD.62.024027
[9] DOI: 10.4310/ATMP.1998.v2.n2.a1 · Zbl 0914.53047 · doi:10.4310/ATMP.1998.v2.n2.a1
[10] DOI: 10.1088/0264-9381/18/23/319 · Zbl 0993.83019 · doi:10.1088/0264-9381/18/23/319
[11] DOI: 10.1103/PhysRevD.54.3840 · doi:10.1103/PhysRevD.54.3840
[12] DOI: 10.1103/PhysRevD.26.1281 · doi:10.1103/PhysRevD.26.1281
[13] DOI: 10.1103/PhysRevD.68.044024 · Zbl 1244.83017 · doi:10.1103/PhysRevD.68.044024
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