Quasinormal Modes Beyond Kerr
Aaron Zimmerman, Huan Yang, Zachary Mark, Yanbei Chen, Luis Lehner
TL;DR
This paper presents a method to compute quasinormal modes of black holes slightly deformed from Kerr, enabling analysis of external influences or alternative gravity theories on black hole oscillations.
Contribution
It introduces a new computational approach for QNMs in nearly Kerr spacetimes, extending understanding beyond ideal Kerr black holes.
Findings
Method applicable to deformed black hole spacetimes
Analysis of scalar field instability in perturbed backgrounds
Frequency shifts in Kerr QNMs due to weak charge
Abstract
The quasinormal modes (QNMs) of a black hole spacetime are the free, decaying oscillations of the spacetime, and are well understood in the case of Kerr black holes. We discuss a method for computing the QNMs of spacetimes which are slightly deformed from Kerr. We mention two example applications: the parametric, turbulent instability of scalar fields on a background which includes a gravitational QNM, and the shifts to the QNM frequencies of Kerr when the black hole is weakly charged. This method may be of use in studies of black holes which are deformed by external fields or are solutions to alternative theories of gravity.
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