Effective tidal deformability of the binary system as a function of the primary mass, m₁, when the chirp mass is held fixed at ﹩{{ \mathcal M }}_{c}=1.188\,{M}_{\odot }﹩. We calculate ﹩\widetilde{{\rm{\Lambda }}}﹩ for three fixed radii, R = 10, 11, and 12 km, shown in purple, blue, and green, respectively. The solid lines show the tidal deformability calculated using the empirically fit universal relation between the tidal deformability of each neutron star and its compactness from Yagi & Yunes (2017), while the dashed lines show the quasi-Newtonian approximation for ﹩{{\rm{\Lambda }}}_{i}﹩ from Equation (7). The quasi-Newtonian approximation is a good approximation to the fully relativistic result.