Extreme Mass Ratio Binary: Radiation reaction and gravitational waveform

TL;DR

This paper reviews recent theoretical advances in modeling gravitational waveforms from extreme mass ratio binaries, crucial for LISA's detection capabilities, by approximating the system as a perturbation of a Kerr black hole.

Contribution

It presents recent progress in calculating gravitational waveforms from extreme mass ratio binaries using Kerr black hole perturbation theory.

Findings

Improved waveform models for supermassive black hole and stellar mass object systems.

Enhanced accuracy in gravitational wave predictions for LISA detection.

Theoretical framework for perturbative analysis of Kerr black holes.

Abstract

For a successful detection of gravitational waves by LISA, it is essential to construct theoretical waveforms in a reliable manner. We discuss gravitational waves from an extreme mass ratio binary system which is expected to be a promising target of the LISA project. The extreme mass ratio binary is a binary system of a supermassive black hole and a stellar mass compact object. As the supermassive black hole dominates the gravitational field of the system, we suppose that the system might be well approximated by a metric perturbation of a Kerr black hole. We discuss a recent theoretical progress in calculating the waveforms from such a system.