Post-Newtonian Quasicircular Initial Orbits for Numerical Relativity

Abstract

We use post-Newtonian (PN) approximations to determine the initial orbital and spin parameters of black hole binaries that lead to low-eccentricity inspirals when evolved with numerical relativity techniques. In particular, we seek initial configurations that lead to very small eccentricities at small separations, as is expected for astrophysical systems. We consider three cases: (i) quasicircular orbits with no radial velocity, (ii) quasicircular orbits with an initial radial velocity determined by radiation reaction, and (iii) parameters obtained form evolution of the PN equations of motion from much larger separations. We study seven cases of spinning, nonprecessing, unequal mass binaries. We then use several definitions of the eccentricity, based on orbital separations and waveform phase and amplitude, and find that using the complete 3PN Hamiltonian for quasicircular orbits to obtain the tangential orbital momentum, and using the highest-known-order radiation reaction expressions to obtain the radial momentum, leads to the lowest eccentricity. The accuracy of this method even exceeds that of inspiral data based on 3PN and 4PN evolutions.

14 pages, 4 figures

References in corpus (24)

• Reducing orbital eccentricity in binary black hole simulations
• Hamiltonian of two spinning compact bodies with next-to-leading order gravitational spin-orbit coupling
• Spin Flips and Precession in Black-Hole-Binary Mergers
• Binary-black-hole initial data with nearly-extremal spins
• Fourth post-Newtonian effective one-body dynamics
• High-spin binary black hole mergers
• Effective-one-body waveforms calibrated to numerical relativity simulations: coalescence of non-precessing, spinning, equal-mass black holes
• Circular orbits and spin in black-hole initial data
• Energy and periastron advance of compact binaries on circular orbits at the fourth post-Newtonian order
• Comparison of Numerical and Post-Newtonian Waveforms for Generic Precessing Black-Hole Binaries
• ADM canonical formalism for gravitating spinning objects
• Reducing eccentricity in black-hole binary evolutions with initial parameters from post-Newtonian inspiral
• Leading order finite size effects with spins for inspiralling compact binaries
• Equivalence of ADM Hamiltonian and Effective Field Theory approaches at next-to-next-to-leading order spin1-spin2 coupling of binary inspirals
• Foundations of multiple black hole evolutions
• Higher-order-in-spin interaction Hamiltonians for binary black holes from Poincaré invariance
• Modeling the source of GW150914 with targeted numerical-relativity simulations
• Tidal heating and torquing of a Kerr black hole to next-to-leading order in the tidal coupling
• Measuring orbital eccentricity and periastron advance in quasi-circular black hole simulations
• Black hole puncture initial data with realistic gravitational wave content
• Flip-flopping binary black holes
• An efficient iterative method to reduce eccentricity in numerical-relativity simulations of compact binary inspiral
• Accuracy Issues for Numerical Waveforms
• Accuracy of the post-Newtonian approximation. II. Optimal asymptotic expansion of the energy flux for quasicircular, extreme mass-ratio inspirals into a Kerr black hole

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• Evolutions of unequal mass, highly spinning black hole binaries
• Eccentricity estimation from initial data for Numerical Relativity Simulations
• Second MAYA Catalog of Binary Black Hole Numerical Relativity Waveforms
• Data-driven extraction, phenomenology and modeling of eccentric harmonics in binary black hole merger waveforms
• Post-Newtonian theory-inspired framework for characterizing eccentricity in gravitational waveforms
• Initial Data and Eccentricity Reduction Toolkit for Binary Black Hole Numerical Relativity Waveforms
• Characterizing the effect of eccentricity on the dynamics of binary black hole mergers in numerical relativity
• A complete waveform comparison of post-Newtonian and numerical relativity in eccentric orbits
• Unveiling the electrodynamic nature of spacetime collisions
• Quasi-Normal Mode Ringing of Binary Black Hole Mergers in Scalar-Gauss-Bonnet Gravity
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