Comparisons of eccentric binary black hole simulations with post-Newtonian models

Details Comparisons of eccentric binary black hole simulations with post-Newtonian models Comparisons of eccentric binary black hole simulations with post-Newtonian models

2008-06-05

arxiv.org/abs/0806.1037v2

Phys. Rev. D 82, 024033 (2010)

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

15 pages, 7 figures. Replaced extrapolation of fit parameters with values at earliest time - results unchanged. Corrected equa

Scientific paper

10.1103/PhysRevD.82.024033

We present the first comparison between numerical relativity (NR) simulations of an eccentric binary black hole system with corresponding post-Newtonian (PN) results. We evolve an equal-mass, non-spinning configuration with an initial eccentricity e ~ 0.1 for 21 gravitational wave cycles before merger, and find agreement in the gravitational wave phase with an adiabatic eccentric PN model with 2 PN radiation reaction within 0.1 radians for 10 cycles. The NR and PN phase difference grows to 0.7 radians by 5 cycles before merger. We find that these results can be obtained by expanding the eccentric PN expressions in terms of the frequency-related variable x = (omega M)^{2/3} with M the total mass of the binary. When using instead the mean motion n = 2 \pi /P, where P is the orbital period, the comparison leads to significant disagreements with NR.

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