  We use a smoothed particle hydrodynamics (SPH) code to examine the effects of
a binary companion on a Be star disk for a range of disk viscosities and
misalignment angles, i.e. the angle between the orbital plane and the primary's
spin axis. The density structures in the disk due to the tidal interaction with
the binary companion are investigated. Expanding on our previous work, the
shape and density structure of density enhancements due to the binary companion
are analyzed and the changes in observed interferometric features due to these
orbiting enhancements are also predicted. We find that larger misalignment
angles and viscosity values result in more tightly wound spiral arms with
densities that fall-off more slowly with radial distance from the central star.
We show that the orbital phase has very little effect on the structure of the
spiral density enhancements. We demonstrate that these spiral features can be
detected with an interferometer in H$\alpha$ and K-band emission. We also show
that the spiral features affect the axis ratios determined by interferometry
depending on the orientation of these features and the observer. For example,
our simulations show that the axis ratios can vary by 20% for our co-planar
binary disk system depending on the location of the disk density enhancements.
