Comparison between numerical-relativity and post-Newtonian waveforms from spinning binaries: the orbital hang-up case

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dc.creatorHannam, Mark
dc.creatorHusa, Sascha
dc.creatorBrügmann, Bernd
dc.creatorGopakumar, Achamveedu
dc.date2007-12-21
dc.date2008-11-26
dc.date.accessioned2026-07-07T11:54:48Z
dc.date.available2026-07-07T11:54:48Z
dc.descriptionWe compare results from numerical simulations of spinning binaries in the "orbital hangup" case, where the binary completes at least nine orbits before merger, with post-Newtonian results using the approximants TaylorT1, T4 and Et. We find that, over the ten cycles before the gravitational-wave frequency reaches $Mω= 0.1$, the accumulated phase disagreement between NR and 2.5PN results is less than three radians, and is less than 2.5 radians when using 3.5PN results. The amplitude disagreement between NR and restricted PN results increases with the black holes' spin, from about 6% in the equal-mass case to 12% when the black holes' spins are $S_i/M_i^2 = 0.85$. Finally, our results suggest that the merger waveform will play an important role in estimating the spin from such inspiral waveforms.
dc.description10 pages, 6 figures. Matches version published in PRD
dc.identifierhttps://arxiv.org/abs/0712.3787
dc.identifierhttp://arxiv.org/abs/0712.3787
dc.identifierPhys.Rev.D78:104007,2008
dc.identifierdoi:10.1103/PhysRevD.78.104007
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/205036
dc.subjectGeneral Relativity and Quantum Cosmology
dc.titleComparison between numerical-relativity and post-Newtonian waveforms from spinning binaries: the orbital hang-up case
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