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

Gopakumar, Achamveedu; Hannam, Mark; Husa, Sascha; Brügmann, Bernd

doi:10.1103/PhysRevD.78.064026

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

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Husa, Sascha
Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

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Citation

Gopakumar, A., Hannam, M., Husa, S., & Brügmann, B. (2008). Comparison between numerical relativity and a new class of post-Newtonian gravitational-wave phase evolutions: The nonspinning equal-mass case. Physical Review D, 78(6): 064026. doi:10.1103/PhysRevD.78.064026.

Cite as: https://hdl.handle.net/11858/00-001M-0000-0013-13A1-8

Abstract

We 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 Momega=0.0455 to Momega=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.