  X-ray-emitting symbiotic stars exhibit a variety of spectral shapes
classified as $\alpha$, $\beta$, $\gamma$, $\delta$ and $\beta$/$\delta$ types,
which have been attributed to different phenomena such as thermonuclear burning
on the surface of the white dwarf (WD) component, shocks between winds and jets
with the red giant companion's extended atmosphere, the presence of heavily
extinguished hot plasma from the inner region from an accretion disk and/or a
combination of these. However, there is observational evidence that this
classification scheme is not definite and, for example, some sources change
from one type to another within months or years. In this work, it is proposed
that a simple disk-like model can be used to explain the X-ray properties
observed from reflection dominated symbiotic stars. For this purpose we use the
Stellar Kinematics Including Radiative Transfer (SKIRT) code, which has been
recently upgraded to include radiative transfer from X-ray photons. It is found
that thee properties of the accretion disk (geometry and density) in
combination with the viewing angle can be invoke to explain the spectral
properties of $\beta$, $\delta$ and $\beta/\delta$ X-ray-emitting symbiotic
stars. Spectral variations and type swaps observed for some X-ray-emitting
sources can also be explained by variations in the disk properties.
