Comparison between numerical relativity and a new class of post-Newtonian gravitational-wave phase evolutions: the non-spinning equal-mass case

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dc.creatorGopakumar, Achamveedu
dc.creatorHannam, Mark
dc.creatorHusa, Sascha
dc.creatorBrügmann, Bernd
dc.date2007-12-21
dc.date.accessioned2026-07-07T12:45:47Z
dc.date.available2026-07-07T12:45:47Z
dc.descriptionWe compare the phase evolution of equal-mass nonspinning black-hole binaries from numerical relativity (NR) simulations with post-Newtonian (PN) results obtained from three PN approximants: the TaylorT1 and T4 approximants, for which NR-PN comparisons have already been performed in the literature, and the recently proposed approximant TaylorEt. The accumulated phase disagreement between NR and PN results over the frequency range $Mω= 0.0455$ to $Mω= 0.1$ is greater for TaylorEt than either T1 or T4, but has the attractive property of decreasing monotonically as the PN order is increased.
dc.description6 pages, 4 figures
dc.identifierhttps://arxiv.org/abs/0712.3737
dc.identifierhttp://arxiv.org/abs/0712.3737
dc.identifierPhys.Rev.D78:064026,2008
dc.identifierdoi:10.1103/PhysRevD.78.064026
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/221165
dc.subjectGeneral Relativity and Quantum Cosmology
dc.titleComparison between numerical relativity and a new class of post-Newtonian gravitational-wave phase evolutions: the non-spinning equal-mass case
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