  We investigate variations in the linear polarization as well as in the V-band
and B-band colour-magnitudes for classical Be star disks. We present two
models: disks with enhanced disk density and disks that are tilted or warped
from the stellar equatorial plane. In both cases, we predict variation in
observable properties of the system as the disk rotates. We use a non-LTE
radiative transfer code BEDISK (Sigut & Jones) in combination with a Monte
Carlo routine that includes multiple scattering (Halonen et al.) to model
classical Be star systems. We find that a disk with an enhanced density region
that is one order of magnitude denser than the disk's base density shows as
much as $\sim$0.2% variability in the polarization while the polarization
position angle varies by $\sim$8\deg. The $\Delta$V magnitude for the same
system shows variations of up to $\sim$0.4 magnitude while the $\Delta$(B-V)
colour varies by at most $\sim$0.01 magnitude. We find that disks tilted from
the equatorial plane at small angles of $\sim$30\deg more strongly reflect the
values of polarization and colour-magnitudes reported in the literature than
disks tilted at larger angles. For this model, the linear polarization varies
by $\sim$0.3%, the polarization position angle varies by $\sim$60\deg, the
$\Delta$V magnitude varies up to 0.35 magnitude, and the $\Delta$(B-V) colour
varies up to 0.1 magnitude. We find that the enhanced disk density models show
ranges of polarization and colour-magnitudes that are commensurate with what is
reported in the literature for all sizes of the density enhanced regions. From
this, we cannot determine any preference for small or large density enhanced
regions.
