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Simulations of black-hole binaries with unequal masses or non-precessing spins: accuracy, physical properties, and comparison with post-Newtonian results

Hannam, M., Husa, S., Ohme, F., Mueller, D., & Bruegmann, B. (2010). Simulations of black-hole binaries with unequal masses or non-precessing spins: accuracy, physical properties, and comparison with post-Newtonian results. Physical Review D., 82(12): 124008. doi:10.1103/PhysRevD.82.124008.

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Genre: Journal Article

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1007.4789 (Preprint), 2MB
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### Creators

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Creators:
Hannam, Mark, Author
Husa, Sascha1, Author
Ohme, Frank1, Author
Mueller, Doreen, Author
Bruegmann, Bernd, Author
Affiliations:
1Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society, escidoc:24013

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Free keywords: General Relativity and Quantum Cosmology, gr-qc
Abstract: We present gravitational waveforms for the last orbits and merger of black-hole-binary (BBH) systems along two branches of the BBH parameter space: equal-mass binaries with equal non-precessing spins, and nonspinning unequal-mass binaries. The waveforms are calculated from numerical solutions of Einstein's equations for black-hole binaries that complete between six and ten orbits before merger. Along the equal-mass spinning branch, the spin parameter of each BH is $\chi_i = S_i/M_i^2 \in [-0.85,0.85]$, and along the unequal-mass branch the mass ratio is $q =M_2/M_1 \in [1,4]$. We discuss the construction of low-eccentricity puncture initial data for these cases, the properties of the final merged BH, and compare the last 8-10 GW cycles up to $M\omega = 0.1$ with the phase and amplitude predicted by standard post-Newtonian (PN) approximants. As in previous studies, we find that the phase from the 3.5PN TaylorT4 approximant is most accurate for nonspinning binaries. For equal-mass spinning binaries the 3.5PN TaylorT1 approximant (including spin terms up to only 2.5PN order) gives the most robust performance, but it is possible to treat TaylorT4 in such a way that it gives the best accuracy for spins $\chi_i > -0.75$. When high-order amplitude corrections are included, the PN amplitude of the $(\ell=2,m=\pm2)$ modes is larger than the NR amplitude by between 2-4%.

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Dates: 2010-07-272010
Publication Status: Published in print
Pages: 20 pages, 9 figures, 6 tables
Publishing info: -
Rev. Method: -
Identifiers: arXiv: 1007.4789
URI: http://arxiv.org/abs/1007.4789
DOI: 10.1103/PhysRevD.82.124008
Degree: -

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### Source 1

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Title: Physical Review D.
Other : Phys. Rev. D.
Source Genre: Journal
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Publ. Info: Lancaster, Pa. : Published for the American Physical Society by the American Institute of Physics
Pages: - Volume / Issue: 82 (12) Sequence Number: 124008 Start / End Page: - Identifier: ISSN: 0556-2821
CoNE: http://pubman.mpdl.mpg.de/cone/journals/resource/111088197762258