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The evolution of global binary black holes variables such as energy or linearmomentum are mainly obtained by applying numerical methods near coalescence,post-Newtonian (PN) expansions, or a combination of both. In this paper, we usea fully relativistic formalism presented several years ago that only usesglobal variables defined at null infinity together with the gravitationalradiation emitted by the source to obtain the time evolution of such variablesfor binary black holes (BBH) systems. For that, we use the Rochester catalogcomposed of 776 BBHs simulations. We compute the final velocity, radiatedenergy, and intrinsic angular momentum predicted by the dynamical equations inthis formalism for nonspinning, aligned and antialigned spins, and severaldifferent precessing configurations. We compare obtained values with reportedvalues in numerical simulations. As BBHs parameter space is still notcompletely covered by numerical simulations, we fit phenomenological formulasfor practical applications to the radiated energy and final velocitiesobtained. Also, we compare the fits with reported values. In conclusion, we seethat our formulae and correlations for the variables described in this work areconsistent with those found in the general literature.

Final velocity and radiated energy in numerical simulations of binary black holes