Gravitational radiation from radial infall of a particle into a Schwarzschild black hole. A numerical study of the spectra, quasi-normal modes and power-law tails

Abstract

The computation of the gravitational radiation emitted by a particle falling into a Schwarzschild black hole is a classic problem studied already in the 1970s. Here we present a detailed numerical analysis of the case of radial infall starting at infinity with no initial velocity. We compute the radiated waveforms, spectra and energies for multipoles up to l = 6, improving significantly on the numerical accuracy of existing results. This is done by integrating the Zerilli equation in the frequency domain using the Green's function method. The resulting wave exhibits a "ring-down" phase whose dominant contribution is a superposition of the quasi-normal modes of the black hole. The numerical accuracy allows us to recover the frequencies of these modes through a fit of that part of the wave. Comparing with direct computations of the quasi-normal modes we reach a \sim 10^{-4} to \sim 10^{-2} accuracy for the first two overtones of each multipole. Our numerical accuracy also allows us to display the power-law tail that the wave develops after the ring-down has been exponentially cut-off. The amplitude of this contribution is \sim 10^2 to \sim 10^3 times smaller than the typical scale of the wave.

15 pages, 7 figures

References in corpus (5)

• Inspiral, merger and ring-down of equal-mass black-hole binaries
• Inspiral, merger and ringdown of unequal mass black hole binaries: a multipolar analysis
• The physical interpretation of the spectrum of black hole quasinormal modes
• Faithful Effective-One-Body waveforms of small-mass-ratio coalescing black-hole binaries
• Comparing Effective-One-Body gravitational waveforms to accurate numerical data

Cited by in corpus (1)

• Horizon-absorption effects in coalescing black-hole binaries: An effective-one-body study of the non-spinning case