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Quasi-Normal Modes of Brane-Localised Standard Model Fields II: Kerr Black Holes
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Quasi-Normal Modes of Brane-Localised Standard Model Fields II: Kerr Black Holes
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This paper presents a comprehensive study of the fundamental quasinormal modes of all Standard Model fields propagating on a brane embedded in a higher-dimensional rotating black hole spacetime. The equations of motion for fields with spin $s=0, 1/2$ and 1 propagating in the induced-on-the-brane background are solved numerically, and the dependence of their QN spectra on the black hole angular momentum and dimensionality of spacetime is investigated. It is found that the brane-localised field perturbations are longer-lived when the higher-dimensional black hole rotates faster, while an increase in the number of transverse-to-the-brane dimensions reduces their lifetime. Finally, the quality factor $Q$, that determines the best oscillator among the different field perturbations, is investigated and found to depend on properties of both the particular field studied (spin, multipole numbers) and the gravitational background (dimensionality, black hole angular momentum number).
Forward citations
Cited by 13 Pith papers
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Two types of quasinormal modes of Casadio-Fabbri-Mazzacurati brane-world black holes
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Direct numerical greybodies for Simpson–Visser and CFM black holes near wormhole endpoints cut residual Hawking luminosity far below WKB estimates, raising a sample lifetime coefficient by ~85.
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Hawking Emission from Black Holes Evaporating toward Wormholes and the Accuracy of the WKB Approximation
Near the wormhole endpoint, the WKB approximation misestimates Hawking luminosities by orders of magnitude; direct numerical greybody factors lengthen an illustrative lifetime estimate by a factor of about 85.
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Quasinormal Spectra of Fields of Various Spin in Asymptotically de Sitter Black Holes within Generalized Proca Theory
Quasinormal frequencies for massless fields in Proca-hairy de Sitter black holes show scalar ℓ=0 modes most sensitive to hair parameter Q, with damping weakening near the three-horizon regime.
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