Abstract
The odd parity gravitational quasi-normal mode spectrum of black holes with non-trivial scalar hair in Horndeski gravity is investigated. We study ‘almost’ Schwarzschild black holes such that any modifications to the spacetime geometry (including the scalar field profile) are treated as small quantities. A modified Regge–Wheeler style equation for the odd parity gravitational degree of freedom is presented to quadratic order in the scalar hair and spacetime modifications, and a parameterisation of the modified quasi-normal mode spectrum is calculated. In addition, statistical error estimates for the new hairy parameters of the black hole and scalar field are given.
Highlights
Gravitational wave (GW) astronomy is in full swing, thanks to numerous and frequent observations of compact object mergers by advanced LIGO and VIRGO [1]
As various observations appear to suggest that black holes are well described by the suite of general relativity (GR) solutions [26, 46], this approach seems sensible. In this way we can treat the new modi ed quasi-normal modes (QNMs) spectrum of these hairy black holes as a small correction to the original GR spectrum, greatly simplifying the analytical and numerical analysis. This is analogous to the study of slowly rotating black holes, where the Kerr background solution is treated as a small modi cation to the Schwarzschild metric, and gravitational wave perturbations are studied on top of this new background
In this paper we have studied the QNMs associated with odd parity gravitational perturbations of spherically symmetric black holes in Horndeski gravity
Summary
Gravitational wave (GW) astronomy is in full swing, thanks to numerous and frequent observations of compact object mergers by advanced LIGO and VIRGO [1]. In this way we can treat the new modi ed QNM spectrum of these hairy black holes as a small correction to the original GR spectrum, greatly simplifying the analytical and numerical analysis This is analogous to the study of slowly rotating black holes, where the Kerr background solution is treated as a small modi cation to the Schwarzschild metric (with the dimensionless black hole spin considered as an ‘expansion’ parameter), and gravitational wave perturbations are studied on top of this new background (see, for example, [47,48,49,50]).
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