Schmidt, Patricia, Hannam, Mark ![]() |
Abstract
We present a simple method to track the precession of a black-hole-binary system during the inspiral, using only information from the gravitational-wave (GW) signal. Our method consists of locating the frame from which the magnitudes of the (ℓ=2, |m|=2) modes are maximized, which we denote the “quadrupole-aligned” frame. We demonstrate the efficacy of this method when applied to waveforms from numerical simulations. In the test case of an equal-mass nonspinning binary, our method locates the direction of the orbital angular momentum to within (Δθ,Δφ)=(0.05°,0.2°). We then apply the method to a q=M2/M1=3 binary that exhibits significant precession. In general, a spinning binary’s orbital angular momentum L is not orthogonal to the orbital plane. Evidence that our method locates the direction of L rather than the normal of the orbital plane is provided by comparison with post-Newtonian results. Also, we observe that it accurately reproduces similar higher-mode amplitudes to a comparable non-precessing binary, and that the frequency of the (ℓ=2, |m|=2) modes is consistent with the “total frequency” of the binary’s motion. The simple form of the quadrupole-aligned waveform may be useful in attempts to analytically model the inspiral-merger-ringdown signal of precessing binaries, and in standardizing the representation of waveforms for studies of accuracy and consistency of source modelling efforts, both numerical and analytical.
Item Type: | Article |
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Date Type: | Publication |
Status: | Published |
Schools: | Advanced Research Computing @ Cardiff (ARCCA) Physics and Astronomy |
Subjects: | Q Science > QB Astronomy |
Additional Information: | 12 pages. |
Publisher: | American Physical Society |
ISSN: | 1550-7998 |
Last Modified: | 19 Oct 2022 10:53 |
URI: | https://orca.cardiff.ac.uk/id/eprint/25871 |
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