(2004).

Based on the results above, we can find that there is one reliable positive correlation between the line width and the line flux of the double-peaked broad H$\alpha$ for the double-peaked emitter 3C390.3, which is against the expected negative correlation confirmed for the other mapped AGN. The unexpected positive correlation should indicate different structures of BLRs of the double-peaked emitter 3C390.3 and normal broad line AGN.

Discussions and Conclusions
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It is clear that the reliable positive correlation shown in Figure \[fj\_3c390\] for the double-peaked emitter 3C390.3 is against the expected result through the Virialization assumption. Thus the following three questions are mainly considered, what determines the unexpected positive correlation? whether the Virialization assumption is still available for double-peaked emitters? whether the unexpected positive correlation can be found for the other double-peaked emitters?

Accretion Disk Model for Double-Peaked Emitters
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For normal broad line AGN, such as NGC5548, the strong negative correlation of the broad line parameters can be naturally explained by the following simple viewpoint: BLR kinematics are dominated by central gravity (some more recent reviews can be found in Down et al. 2010, Sluse et al. 2011), which could be well appropriate to the broad line Seyfert 