Numerical evolution of the center of mass and angular momentum for binaries black holes

Abstract

The asymptotic approach derived by Kozameh-Quiroga (K-Q) provides a modern framework to obtain the evolution of global variables of isolated sources of gravitational radiation. We test the K-Q formalism evolving the equations of motion for the center of mass, the intrinsic angular momentum, and several other global variables, for black hole binary coalescence. First we evolve the equations of motion using 777 simulations from the RIT catalogue numerical data of ${\psi }_4$ [J. Healy and C.O. Lousto, Third RIT binary black hole simulations catalog, Phys. Rev. D 102, 104018 (2020).]. We then analyze the trajectory of the center of mass and compute the final state of other physical variables after the coalescence has taken place. Finally, we show the results obtained from our equations of motion are consistent with those in the Rochester metadata.

arXiv commentPages: 12. Figures:22

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Cited by in corpus (4)

• Scattering theory with matter fields of classical gravitons in the null surface formulation
• Final velocity and radiated energy in numerical simulations of binary black holes
• Fast Waveform Generation for Gravitational Waves using Evolutionary Algorithms
• The Fourth RIT binary black hole simulations catalog: Extension to Eccentric Orbits