  We model the circumstellar disk of $\delta$ Sco using the 3-dimensional Monte
Carlo radiative transfer code HDUST in order to quantify the large scale
changes in the disk through the years 2000 to 2018, and to see if these changes
can be attributed to the secondary star affecting the disk throughout its
orbit. We determine our best-fitting models through matching simulated
observations to actual H$\rm \alpha$ spectroscopy and V-band photometric
observations. Our modelling results confirm previous findings that the disk of
$\delta$ Sco was forming early in the century. We also find a period of disk
dissipation when the companion is at apastron, as well as a significant growth
of the disk between 2009 and 2011, prior to the periastron of 2011. Due to the
steady-state nature of the disk after 2011, it is difficult to say whether the
variations seen are due to the effect of the close passage of the binary
companion.
