The fraction of the radial distance from the SMBH (logarithmic scale) for cases transitioning from the ADIOS to the ZEBRA state due to kicks, as a function of the SMBH accretion rate (in units of Eddington rate) and SMBH mass in the TQM model. The radial distance ranges from 6 × GM_SMBH/c² to 6 × 10⁷ × GM_SMBH/c², with an assumed BH mass m_BH = 50 M_⊙. Red circles highlight cases where the transition from the ADIOS to the ZEBRA state occurs at the minimum H_AGN/R_BH location, where mergers are more probable. Gray empty circles represent cases where no transition regions appear. We evaluate ﹩{\dot{M}}_{{\rm{out}}}﹩ at uniform logarithmic intervals separated by a factor of 2 for M_SMBH≤10⁷ M_⊙ and ﹩\sqrt{2}﹩ for M_SMBH > 10⁷ M_⊙, where ﹩{\dot{M}}_{{\rm{out}}}﹩ is the inflow rate at the outer boundary (6 × 10⁷ × GM_SMBH/c²). This results in uneven coverage in ﹩{\dot{M}}_{{\rm{SMBH}}}﹩, reflecting its nonlinear dependence on ﹩{\dot{M}}_{{\rm{out}}}﹩. In the TQM model, when the AGN luminosity exceeds ≳10⁴⁴ erg s⁻¹, the transition from the ADIOS to the ZEBRA state is associated with kicks at the minimum H_AGN/R_BH region. We conclude that high-accretion rate, massive SMBHs are the most promising to produce the EM counterparts as discussed here.