Accurate time-domain gravitational waveforms for extreme-mass-ratio binaries

Abstract

The accuracy of time-domain solutions of the inhomogeneous Teukolsky equation is improved significantly. Comparing energy fluxes in gravitational waves with highly accurate frequency-domain results for circular equatorial orbits in Schwarzschild and Kerr, we find agreement to within 1% or better, which we believe can be even further improved. We apply our method to orbits for which frequency-domain calculations have a relative disadvantage, specifically high-eccentricity (elliptical and parabolic) "zoom-whirl" orbits, and find the energy fluxes, waveforms, and characteristic strain in gravitational waves.

6 pages, 9 figures, 2 tables; Changes: some errors corrected. Comparison with Frequency-domain now done in stronger field

References in corpus (1)

• Gravitational wave snapshots of generic extreme mass ratio inspirals

Cited by in corpus (6)

• Towards adiabatic waveforms for inspiral into Kerr black holes: I. A new model of the source for the time domain perturbation equation
• Zoom-Whirl Orbits in Black Hole Binaries
• Towards adiabatic waveforms for inspiral into Kerr black holes: II. Dynamical sources and generic orbits
• Scalar-field perturbations from a particle orbiting a black hole using numerical evolution in 2+1 dimensions
• m-Mode Regularization Scheme for the Self Force in Kerr Spacetime
• Computational Efficiency of Frequency-- and Time--Domain Calculations of Extreme Mass--Ratio Binaries: Equatorial Orbits