Dynamics of spin-2 fields in Kerr background geometries

TL;DR

This paper introduces a numerical method for evolving spin-2 perturbations in Kerr black hole backgrounds, capturing the entire waveform evolution including ringdown and tail phases, aiding understanding of gravitational signals.

Contribution

It presents a new numerical approach for solving the Teukolsky equation in Kerr geometries, explicitly handling radial characteristic directions for black hole perturbations.

Findings

Successfully models the propagation of perturbations through all phases

Provides insights into the influence of black hole spin on gravitational wave signals

Enables detailed analysis of black hole ringdown and tail behaviors

Abstract

We have developed a numerical method for evolving perturbations of rotating black holes. Solutions are obtained by integrating the Teukolsky equation written as a first-order in time, coupled system of equations, in a form that explicitly exhibits the radial characteristic directions. We follow the propagation of generic initial data through the burst, quasi-normal ringing and power-law tail phases. Future results may help to clarify the role of black hole angular momentum on signals produced during the final stages of black hole coalescence.