  The evolution of global binary black holes variables such as energy or linear
momentum are mainly obtained by applying numerical methods near coalescence,
post-Newtonian (PN) expansions, or a combination of both. In this paper, we use
a fully relativistic formalism presented several years ago that only uses
global variables defined at null infinity together with the gravitational
radiation emitted by the source to obtain the time evolution of such variables
for binary black holes (BBH) systems. For that, we use the Rochester catalog
composed of 776 BBHs simulations. We compute the final velocity, radiated
energy, and intrinsic angular momentum predicted by the dynamical equations in
this formalism for nonspinning, aligned and antialigned spins, and several
different precessing configurations. We compare obtained values with reported
values in numerical simulations. As BBHs parameter space is still not
completely covered by numerical simulations, we fit phenomenological formulas
for practical applications to the radiated energy and final velocities
obtained. Also, we compare the fits with reported values. In conclusion, we see
that our formulae and correlations for the variables described in this work are
consistent with those found in the general literature.
