Radiation from low-momentum zoom-whirl orbits

Abstract

We study zoom-whirl behaviour of equal mass, non-spinning black hole binaries in full general relativity. The magnitude of the linear momentum of the initial data is fixed to that of a quasi-circular orbit, and its direction is varied. We find a global maximum in radiated energy for a configuration which completes roughly one orbit. The radiated energy in this case exceeds the value of a quasi-circular binary with the same momentum by 15%. The direction parameter only requires minor tuning for the localization of the maximum. There is non-trivial dependence of the energy radiated on eccentricity (several local maxima and minima). Correlations with orbital dynamics shortly before merger are discussed. While being strongly gauge dependent, these findings are intuitive from a physical point of view and support basic ideas about the efficiency of gravitational radiation from a binary system.

9 pages, 6 figures, Amaldi8 conference proceedings as published

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• Exploring New Physics Frontiers Through Numerical Relativity
• The numerical relativity breakthrough for binary black holes
• Eccentric black hole mergers and zoom-whirl behavior from elliptic inspirals to hyperbolic encounters
• Gravitational waves and mass ejecta from binary neutron star mergers: Effect of large eccentricities
• The Transient Gravitational-Wave Sky
• Initial data for binary neutron stars with adjustable eccentricity
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• Induced Spins from Scattering Experiments of Initially Nonspinning Black Holes
• Spinning compact binary dynamics and chameleon orbits
• Orbiting black-hole binaries and apparent horizons in higher dimensions
• Spin-up and mass-gain in hyperbolic encounters of spinning black holes
• Spin dynamics of moving bodies in rotating black hole spacetimes