A comparison of various characteristic sizes in the TQM model. Solid, dashed, and dotted black lines represent the sizes of the wind, AGN-disk gas, and CBD, respectively. Dashed and dotted cyan lines indicate the wind size limits due to shear from the SMBH (H_Ω) and breakout conditions for ﹩\tau \gt {\beta }_{{\rm{ej}}}^{-1}﹩ (H_τ), respectively. The lines for H_Ω are plotted only where the local Keplerian velocity about the SMBH exceeds the wind velocity. Thick and thin lines denote results considering and neglecting gap formation around BHs, respectively. Since the shock-cooling luminosity is proportional to the size of shocked materials (Equation (17)), these size distributions are useful for understanding the parameters that lead to the production of bright shock-cooling emission. The blue-shaded regions represent where the ADIOS state transitions to the ZEBRA state as a result of kicks at mergers or interactions. The sizes of winds and AGN-disk gas are affected by the SMBH mass, the accretion rate onto the SMBH, the radial location, and the AGN-disk model.