Black-hole binary simulations: The mass ratio 10:1

Abstract

We present the first numerical simulations of an initially nonspinning black-hole binary with mass ratio as large as 10:1 in full general relativity. The binary completes approximately three orbits prior to merger and radiates (0.415±0.017)% of the total energy and (12.48±0.62)% of the initial angular momentum in the form of gravitational waves. The single black hole resulting from the merger acquires a kick of (66.7±3.3) km/s relative to the original center of mass frame. The resulting gravitational waveforms are used to validate existing formulas for the recoil, final spin, and radiated energy over a wider range of the symmetric mass ratio parameter eta=M1M2/(M1+M2)^2 than previously possible. The contributions of [script-l]>2 multipoles are found to visibly influence the gravitational wave signal obtained at fixed inclination angles.

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