1 galaxy NGC5548 (Bentz et al. 2007, Denney et al. 2010, Peterson et al. 2002, 2004, Wanders & Peterson 1996,) and some other mapped broad line AGN (Peterson et al. 2004): stronger continuum emission leads to deeper ionization boundary (larger flux-weighted size of BLR) and leads to smaller general rotating velocity (smaller line width). And then, through the broad line strength being applied to estimate the size of BLR, $R_{BLR}\propto L(H\alpha)^{\sim0.5}$, the negative correlation of the line width and the line flux can be found. Certainly, the viewpoint is not appropriate to the double-peaked emitter 3C390.3.

If the theoretical accretion disk model was accepted, what result about the correlation between the size of BLR and the continuum/line flux should be expected for 3C390.3? In the context of the theoretical disk model for double-peaked emitters, such as the elliptical accretion disk model (Eracleous et al. 1995) which can be well applied to best fit the observed line spectra of 3C390.3 observed around 1995, the disk-like BLR is locating into the central accretion disk, and does share the kinematic characters of the central accretion disk. For 3C390.3, the inner and outer boundary radii of the elliptical disk-like BLR are about $R_{in}\sim150 - 