  Analyzing the observations obtained by the LIGO and the Virgo Collaborations,
a new era has begun in binary black hole (BBH) merger processes and black hole
physics studies. The fact that very massive stars that will become black holes
at the end of their evolution are in binary or multiple states adds particular
importance to BBH studies. In this study, using the SEOBNRv4$\_opt$
gravitational waveform model developed for compact binary systems, many ($\sim
10^6$) models were produced under different initial conditions, and the pre-
and post-merge parameters were compared. In the models, it is assumed that the
initial total mass (M$_{\rm{tot}}$) of the binary systems varies between 12-130
$\rm{M}_\odot$ with step interval 1$\rm{M}_\odot$, the mass ratios ($q =
\rm{m}_{1i}/\rm{m}_{2i}$) vary between 1 and 2 with step interval 0.004, and
the initial spin ($\abs{\rchi_{1i}} = \abs{\rchi_{2i}}$) value varies between
$-0.83$ and $+0.83$ with step interval 0.017. Final spin ($\rchi_{f}$),
fractional mass loss (M$_{FL}$), and the maximum gravitational wave amplitude
(h$_{\rm{max}}$) obtained during the merger were compared with appropriate
tables and figures obtained from the results of the relativistic numeric model
obtained according to the initial parameters. Our results show that
M$_{\rm{FL}}$ in generated BBH coalescences varied about 2.7 to 9.2\%, and
$\rchi_{\rm{f}}$ between 0.29 and 0.91. In most of the BBHs we have modeled, we
found that M$_{\rm{FL}}$ varies inversely with $q$. However, it has been found
that M$_{\rm{FL}}$ values are not always inversely varied to the $q$ parameter
in systems of opposite initial spin, where the large mass black hole component
is positively oriented. Accordingly, it is understood that the values of
M$_{\rm{FL}}$ decrease to a certain point of $q$ and then increase according to
the increasing direction of $q$.
