Black hole perturbation theory and gravitational wave source modelling

Central to the gravitational wave detections by the current LIGO-Virgo-KAGRA network of ground based detectors, has been the underlying analytical and numerical models of binary systems of compact objects (black holes, neutron stars or combinations thereof). With future space based detectors such as LISA, new sources of gravitational waves will necessitate the need for new analytical models. One such source are extreme mass-ratio inspirals, where a ~10 solar mass compact object orbits a galactic-centre type massive black hole of ~10^6 solar masses.

In this talk I will overview the role of black hole perturbation theory in describing these objects using the gravitational self-force approach, with an emphasis on the relation to other analytical approaches to two-body dynamics in general relativity. I will also discuss the use of analytic perturbation theory to describe gravitational wave scattering in black hole spacetimes, and the relation between this problem and scattering amplitudes for massive spinning particles in quantum field theory.

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