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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 holephysics studies. The fact that very massive stars that will become black holesat the end of their evolution are in binary or multiple states adds particularimportance to BBH studies. In this study, using the SEOBNRv4$\_opt$gravitational waveform model developed for compact binary systems, many ($\sim10^6$) models were produced under different initial conditions, and the pre-and post-merge parameters were compared. In the models, it is assumed that theinitial 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, andthe 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 appropriatetables and figures obtained from the results of the relativistic numeric modelobtained according to the initial parameters. Our results show thatM$_{\rm{FL}}$ 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, wefound that M$_{\rm{FL}}$ varies inversely with $q$. However, it has been foundthat M$_{\rm{FL}}$ values are not always inversely varied to the $q$ parameterin systems of opposite initial spin, where the large mass black hole componentis positively oriented. Accordingly, it is understood that the values ofM$_{\rm{FL}}$ decrease to a certain point of $q$ and then increase according tothe increasing direction of $q$.

The spin and mass ratio affects the gravitational waveforms of binary black hole mergers with a total system mass of 12-130 $\rm{M}_\odot$