  We examine the evolution of the disk surrounding the Be star in the highly
eccentric binary system $\delta$ Scorpii over its three most recent periastron
passages. $V$-band and $B-V$ photometry, along with H$\alpha$ spectroscopy are
combined with a new set of extensive multi-band polarimetry data to produce a
detailed comparison of the disk's physical conditions during the time periods
surrounding each closest approach of the secondary star. We use the
three-dimensional Monte Carlo radiative transfer code \textsc{HDUST} and
smoothed particle hydrodynamics (\textsc{SPH}) code to support our observations
with models of disk evolution, discussing the behaviour of the H$\alpha$ and
He\,\textsc{i} 6678 lines, $V$-band magnitude, and polarization degree. We
compare the characteristics of the disk immediately before each periastron
passage to create a baseline for the unperturbed disk. We find that the extent
of the H$\alpha$ emitting region increased between each periastron passage, and
that transient asymmetries in the disk become more pronounced with each
successive encounter. Asymmetries of the H$\alpha$ and He\,\textsc{i} 6678
lines in 2011 indicate that perturbations propagate inward through the disk
near periastron. When the disk's direction of orbit is opposite to that of the
secondary, the parameters used in our models do not produce spiral density
enhancements in the H$\alpha$ emitting region because the tidal interaction
time is short due to the relative velocities of the disk particles with the
secondary. The effects of the secondary star on the disk are short-lived and
the disk shows independent evolution between each periastron event.
