Dynamical decay times, ﹩t_{\mathrm{dyn}\,}﹩, of BMBHs from ﹩a_{h}﹩ to ﹩a_{\mathrm{GW}\,}﹩ as a function of the BMBH mass (the time to final GW‐induced decay, ﹩t_{\mathrm{GW}\,}﹩, from ﹩a_{\mathrm{GW}\,}﹩ to ﹩a=0﹩ is negligible compared to the initial dynamical decay phase). Different merger scenarios are shown (Table 3): major mergers (solid line), minor mergers (dashed line), and elliptical mergers (dash‐dotted line). Without MPs (crosses, for ﹩Q=1﹩), the decay times are longer than the age of the universe (horizontal line) for all BMBH mass in this range.