  We report on the radio quiet quasar SDSS J2125-0813 which obviously emits
optical FeII emission lines and double-peaked broad Balmer emission lines.
Using the accretion disk model for double-peaked broad low-ionization emission
lines, we reproduce the composite line spectra at the optical band between
4100$\AA$ and 5600$\AA$. Broad FeII emission lines can be fit simultaneously
with the broad H$\beta$ and MgI lines, such that all broad lines have an
elliptical disk profile with the same disk parameters. This results indicates
that the optical FeII emission lines originate from the accretion disk near the
central black hole which produces the double-peaked broad Balmer emission
lines. Furthermore, we find that the object has dimensionless accretion rate
$\dot{m}\sim0.4-0.6$ which is much larger than accretion rate for ADAF mode,
and that the energy budget of the accretion disk is enough to power the
double-peaked broad Balmer emission lines.
