We study analytically the quasinormal mode spectrum of near-extremal (rotating) Kerr black holes. We find an analytic expression for these black-hole resonances in terms of the black-hole physical parameters: its Bekenstein–Hawking temperature, T BH , and its horizon's angular velocity, Ω. The expression is valid in the intermediate asymptotic regime 1 ≪ |ω| ≪ T −1 BH .
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Uri Keshet (2005) studied this question.
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