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Title: Binary black hole coalescence in the extreme-mass-ratio limit: Testing and improving the effective-one-body multipolar waveform

Abstract

We discuss the properties of the effective-one-body (EOB) multipolar gravitational waveform emitted by nonspinning black-hole binaries of masses {mu} and M in the extreme-mass-ratio limit {mu}/M={nu}<<1. We focus on the transition from quasicircular inspiral to plunge, merger, and ringdown. We compare the EOB waveform to a Regge-Wheeler-Zerilli waveform computed using the hyperboloidal layer method and extracted at null infinity. Because the EOB waveform keeps track analytically of most phase differences in the early inspiral, we do not allow for any arbitrary time or phase shift between the waveforms. The dynamics of the particle, common to both wave-generation formalisms, is driven by a leading-order O({nu}) analytically resummed radiation reaction. The EOB and the Regge-Wheeler-Zerilli waveforms have an initial dephasing of about 5x10{sup -4} rad and maintain then a remarkably accurate phase coherence during the long inspiral ({approx}33 orbits), accumulating only about -2x10{sup -3} rad until the last stable orbit, i.e. {Delta}{phi}/{phi}{approx}-5.95x10{sup -6}. We obtain such accuracy without calibrating the analytically resummed EOB waveform to numerical data, which indicates the aptitude of the EOB waveform for studies concerning the Laser Interferometer Space Antenna. We then improve the behavior of the EOB waveform around merger by introducing and tuning next-to-quasicircular corrections in bothmore » the gravitational wave amplitude and phase. For each multipole we tune only four next-to-quasicircular parameters by requiring compatibility between EOB and Regge-Wheeler-Zerilli waveforms at the light ring. The resulting phase difference around the merger time is as small as {+-}0.015 rad, with a fractional amplitude agreement of 2.5%. This suggest that next-to-quasicircular corrections to the phase can be a useful ingredient in comparisons between EOB and numerical-relativity waveforms.« less

Authors:
 [1];  [2];  [3]
  1. Theoretical Physics Institute, University of Jena, 07743 Jena (Germany)
  2. Institut des Hautes Etudes Scientifiques, 91440 Bures-sur-Yvette (France)
  3. Theoretical Astrophysics, California Institute of Technology, Pasadena, California 91125 (United States)
Publication Date:
OSTI Identifier:
21537530
Resource Type:
Journal Article
Journal Name:
Physical Review. D, Particles Fields
Additional Journal Information:
Journal Volume: 83; Journal Issue: 6; Other Information: DOI: 10.1103/PhysRevD.83.064010; (c) 2011 American Institute of Physics; Journal ID: ISSN 0556-2821
Country of Publication:
United States
Language:
English
Subject:
72 PHYSICS OF ELEMENTARY PARTICLES AND FIELDS; 79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ACCURACY; AMPLITUDES; BINARY STARS; BLACK HOLES; COALESCENCE; COMPARATIVE EVALUATIONS; COMPATIBILITY; CORRECTIONS; GRAVITATIONAL WAVES; INTERFEROMETERS; LAYERS; MASS; PARTICLES; PHASE SHIFT; SPACE; WAVE FORMS; EVALUATION; MEASURING INSTRUMENTS; STARS

Citation Formats

Bernuzzi, Sebastiano, Nagar, Alessandro, and Zenginoglu, Anil. Binary black hole coalescence in the extreme-mass-ratio limit: Testing and improving the effective-one-body multipolar waveform. United States: N. p., 2011. Web. doi:10.1103/PHYSREVD.83.064010.
Bernuzzi, Sebastiano, Nagar, Alessandro, & Zenginoglu, Anil. Binary black hole coalescence in the extreme-mass-ratio limit: Testing and improving the effective-one-body multipolar waveform. United States. https://doi.org/10.1103/PHYSREVD.83.064010
Bernuzzi, Sebastiano, Nagar, Alessandro, and Zenginoglu, Anil. Tue . "Binary black hole coalescence in the extreme-mass-ratio limit: Testing and improving the effective-one-body multipolar waveform". United States. https://doi.org/10.1103/PHYSREVD.83.064010.
@article{osti_21537530,
title = {Binary black hole coalescence in the extreme-mass-ratio limit: Testing and improving the effective-one-body multipolar waveform},
author = {Bernuzzi, Sebastiano and Nagar, Alessandro and Zenginoglu, Anil},
abstractNote = {We discuss the properties of the effective-one-body (EOB) multipolar gravitational waveform emitted by nonspinning black-hole binaries of masses {mu} and M in the extreme-mass-ratio limit {mu}/M={nu}<<1. We focus on the transition from quasicircular inspiral to plunge, merger, and ringdown. We compare the EOB waveform to a Regge-Wheeler-Zerilli waveform computed using the hyperboloidal layer method and extracted at null infinity. Because the EOB waveform keeps track analytically of most phase differences in the early inspiral, we do not allow for any arbitrary time or phase shift between the waveforms. The dynamics of the particle, common to both wave-generation formalisms, is driven by a leading-order O({nu}) analytically resummed radiation reaction. The EOB and the Regge-Wheeler-Zerilli waveforms have an initial dephasing of about 5x10{sup -4} rad and maintain then a remarkably accurate phase coherence during the long inspiral ({approx}33 orbits), accumulating only about -2x10{sup -3} rad until the last stable orbit, i.e. {Delta}{phi}/{phi}{approx}-5.95x10{sup -6}. We obtain such accuracy without calibrating the analytically resummed EOB waveform to numerical data, which indicates the aptitude of the EOB waveform for studies concerning the Laser Interferometer Space Antenna. We then improve the behavior of the EOB waveform around merger by introducing and tuning next-to-quasicircular corrections in both the gravitational wave amplitude and phase. For each multipole we tune only four next-to-quasicircular parameters by requiring compatibility between EOB and Regge-Wheeler-Zerilli waveforms at the light ring. The resulting phase difference around the merger time is as small as {+-}0.015 rad, with a fractional amplitude agreement of 2.5%. This suggest that next-to-quasicircular corrections to the phase can be a useful ingredient in comparisons between EOB and numerical-relativity waveforms.},
doi = {10.1103/PHYSREVD.83.064010},
url = {https://www.osti.gov/biblio/21537530}, journal = {Physical Review. D, Particles Fields},
issn = {0556-2821},
number = 6,
volume = 83,
place = {United States},
year = {2011},
month = {3}
}