  We present the high resolution spectra of the D type symbiotic stars V1016
Cygni and HM Sagittae obtained with the Bohyunsan Optical Echelle Spectrograph
(BOES), and investigate the double-peaked asymmetric profiles of the Raman
scattered O VI 6825. By adopting a wind accretion disk model, we assume that
the O VI emission region is described by a Keplerian thin disk. The Raman
scattering occurs in a neutral region near the giant, taking in the form of a
slow stellar wind, part of which is ionized by the strong UV radiation from the
hot white dwarf. Using a Monte Carlo technique, we compute the line profiles
that are modulated by the slow spherical stellar wind from the giant component
with the ionization front approximated by a hyperboloid. In order to account
for the asymmetry and the existence of a central dip in the profiles, we add an
O VI resonance scattering region between the hot white dwarf and the giant star
which hinders the incidence of slightly blue O VI photons upon the H I region.
Overall good fits to the observed data are obtained from our model, which lends
support to the accretion disk emission model in these objects. The best fitting
parameters for V1016 Cyg are $v_o=30{\rm km s^{-1}}$,
  $v_\infty=11{\rm km s^{-1}}$, and $v_{c}=10{\rm km s^{-1}}$, where $v_o$,
$v_\infty$ and $v_{c}$ are the velocity of the outer disk rim, the terminal
velocity of the giant wind, and the velocity component of the resonance
scattering O VI region along the binary axis, respectively. Similar fitting
parameters $v_o=27{\rm km s^{-1}}$, $v_\infty=10{\rm km s^{-1}}$ and
$v_{c}=9{\rm km s^{-1}}$ are obtained for HM Sge. We also investigate the
effect of a hot spot in a disk that is well known in accretion disks in
cataclysmic variables.
