Further Evidence for the Accretion Disk Origination of the Double-Peaked
  Broad H$\alpha$ of 3C390.3
  In the letter, under the widely accepted theoretical accretion disk model for
the double-peaked emitter 3C390.3, the extended disk-like BLR can be well split
into ten rings, and then the time lags between the lines from the rings and the
continuum emission are estimated, based on the observed spectra around 1995. We
can find one much strong correlation between the determined time lags (in unit
of light-day) and the flux weighted radii (in unit of ${\rm R_G}$) of the
rings, which is well consistent with the expected results through the
theoretical accretion disk model. Moreover, through the strong correlation, the
black hole masses of 3C390.3 are independently estimated as $\sim10^9{\rm
M_{\odot}}$, the same as the reported black hole masses in the literature. The
consistencies provide further evidence to strongly support the accretion disk
origination of the double-peaked broad balmer lines of 3C390.3.
