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arXiv · 1012.3173

Black-hole binaries go to eleven orbits

Ulrich Sperhake·Bernd Bruegmann·Doreen Mueller·Carlos F. Sopuerta
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Abstract

We analyse an eleven-orbit inspiral of a non-spinning black-hole binary with mass ratio q=M1/M2=4. The numerically obtained gravitational waveforms are compared with post-Newtonian (PN) predictions including several sub-dominant multipoles up to multipolar indices (l=5,m=5). We find that (i) numerical and post-Newtonian predictions of the phase of the (2,2) mode accumulate a phase difference of about 0.35 rad at the PN cut off frequency 0.1 for the Taylor T1 approximant when numerical and PN waveforms are matched over a window in the early inspiral phase; (ii) in contrast to previous studies of equal-mass and specific spinning binaries, we find the Taylor T4 approximant to agree less well with numerical results, provided the latter are extrapolated to infinite extraction radius; (iii) extrapolation of gravitational waveforms to infinite extraction radius is particularly important for subdominant multipoles with l unequal m; (iv) 3PN terms in post-Newtonian multipole expansions significantly improve the agreement with numerical predictions for sub-dominant multipoles.

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Ulrich Sperhake, Bernd Bruegmann, Doreen Mueller, Carlos F. Sopuerta. 2011-06-07. Black-hole binaries go to eleven orbits. https://arxiv.org/abs/1012.3173

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