Properties of flares— luminosity, temperature, and duration— as functions of AGN luminosity at locations where H_AGN/R_BH reaches its minimum, and mergers are more probable. The upper, middle, and lower panels show the ratio of flare luminosity to AGN luminosity (assuming a bolometric correction of 5, F. Duras et al. 2020), the radiation temperature in units of 10⁴ K, and the diffusion timescale in days, respectively. The columns from left to right show results for cooling flares from winds, AGN-disk gas, and CBDs shocked by jets, as well as for cooling and breakout emission from AGN-disk gas shocked by SN explosions. The lines’ styles correspond to different SMBH masses: solid for 10⁶ M_⊙, dashed for 10⁷ M_⊙, and dotted for 10⁸ M_⊙. Blue and orange lines indicate the TQM and SG models, respectively. In the lower panels, the delay time between X-ray and optical emission in AGN variability (Equation (20)) is shown with gray lines. The dashed cyan line indicates f_L,SC = 1, below which flares are too dim to detect. Cooling emission associated with jets from shocked winds and AGN-disk gas can be as bright as host AGN emission for L_AGN ∼ 10⁴⁴ − 10⁴⁵ erg s⁻¹ in the optical-UV bands. Its properties can be used to distinguish different AGN-disk models.