Reducing orbital eccentricity in binary black hole simulations

Details Reducing orbital eccentricity in binary black hole simulations Reducing orbital eccentricity in binary black hole simulations

2007-02-20

arxiv.org/abs/gr-qc/0702106v2

Class.Quant.Grav.24:S59-S82,2007

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

27 pages, 9 figures; various minor clarifications; accepted to the "New Frontiers" special issue of CQG

Scientific paper

10.1088/0264-9381/24/12/S06

Binary black hole simulations starting from quasi-circular (i.e., zero radial velocity) initial data have orbits with small but non-zero orbital eccentricities. In this paper the quasi-equilibrium initial-data method is extended to allow non-zero radial velocities to be specified in binary black hole initial data. New low-eccentricity initial data are obtained by adjusting the orbital frequency and radial velocities to minimize the orbital eccentricity, and the resulting ($\sim 5$ orbit) evolutions are compared with those of quasi-circular initial data. Evolutions of the quasi-circular data clearly show eccentric orbits, with eccentricity that decays over time. The precise decay rate depends on the definition of eccentricity; if defined in terms of variations in the orbital frequency, the decay rate agrees well with the prediction of Peters (1964). The gravitational waveforms, which contain $\sim 8$ cycles in the dominant l=m=2 mode, are largely unaffected by the eccentricity of the quasi-circular initial data. The overlap between the dominant mode in the quasi-circular evolution and the same mode in the low-eccentricity evolution is about 0.99.

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