250{\rm R_G}$ and $R_{out}\sim1100 - 1400{\rm R_G}$, under the theoretical accretion disk model (Eracleous & Halpern 1994, 2003, Flohic & Eracleous 2008, Shapovalova et al. 2001, Zhang 2011a, Paper I). Based on the oversimplified extended disk-like BLR (no considerations of tiny contributions from probable hot spots, warped structures, spiral arms etc. for 3C390.3 around 1995), one simple result can be expected: stronger continuum emission leads to stronger broad line emission coming from the inner part of the disk-like BLR (and then larger line width) in one short period (much shorter than the traveling time for ionizing photons through the whole BLR), because the stronger ionizing continuum firstly reaches the inner part of the disk-like BLR.

In other words, stronger continuum emission (strong line flux) leads to larger flux ratio of the broad H$\alpha$ from the inner part of the BLR to the broad H$\alpha$ from the outer part of the BLR, and leads to larger line width due to larger contributions from the higher velocity clouds in inner part of BLR, which is similar as the results shown in Figure \[fj\_3c390\]. So that, we check the properties of the broad line flux ratio $R = f_{1/2}/f_{all}$, where $f_{1/2}$ means the 