Abstract
The Klein–Gordon equation for a massive scalar field in the background of a rapidly-rotating Kerr black hole is studied analytically. In particular, we derive a simple formula for the stationary (marginally-stable) resonances of the field in the black-hole spacetime. The analytically derived formula is shown to agree with direct numerical computations of the resonances. Our results provide an upper bound on the instability regime of rapidly rotating Kerr black holes to massive scalar perturbations.
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Notes
This statement seems to hold true for all bosonic fields.
In these units μ has the dimensions of 1/length.
We note that, in addition to the bound states of the massive field, the field also has an infinite set of discrete quasinormal resonances [101] which are characterized by outgoing waves at spatial infinity.
In the τ≪1 regime the condition 2β>1 is satisfied by modes with \(m<\sqrt{2l(l+1)/3}\), see Eq. (28) below. In particular, it is satisfied by the fundamental l=m=1 mode.
We denote by ϵ the solution of the quadratic equation (30). The O(ϵ 3) term in (30) is −16(2n+1)ϵ 3. In the τ→0 limit this term introduces a small correction of the form: ϵ→ϵ(1+δ) with \(\delta\simeq{{m^{2}(2n+1)}\over{\ell(\ell+1+2n)^{2}}}\). Note that in the regime 2β>1 that we consider (\(m<\sqrt{2l(l+1)/3}\), see footnote 4), one has \(\delta<{{{2\over 3}l(l+1)}\over{\sqrt{{4\over 3}l(l+1)+1}[\sqrt{{4\over 3}l(l+1)+1}+1]^{2}}}\ll 1\).
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Acknowledgements
This research is supported by the Carmel Science Foundation. I thank Yael Oren, Arbel M. Ongo and Ayelet B. Lata for stimulating discussions.
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Hod, S. Stationary resonances of rapidly-rotating Kerr black holes. Eur. Phys. J. C 73, 2378 (2013). https://doi.org/10.1140/epjc/s10052-013-2378-x
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DOI: https://doi.org/10.1140/epjc/s10052-013-2378-x