  HD 163296 is a Herbig Ae star that underwent a dramatic $\sim$0.8 magnitude
drop in brightness in the V photometric band in 2001 and a brightening in the
near-IR in 2002. Because the star possesses Herbig-Haro objects travelling in
outflowing bipolar jets, it was suggested that the drop in brightness was due
to a clump of dust entrained in a disk wind, blocking the line-on-sight toward
the star. In order to quantify this hypothesis, we investigated the brightness
drop at visible wavelengths and the brightening at near-IR wavelengths of HD
163296 using the Monte Carlo Radiative Transfer Code, HOCHUNK3D. We created
three models to understand the events. Model 1 describes the quiescent state of
the system. Model 2 describes the change in structure that led to the drop in
brightness in 2001. Model 3 describes the structure needed to produce the
observed 2002 brightening of the near-IR wavelengths. Models 2 and 3 utilize a
combination of a disk wind and central bipolar flow. By introducing a filled
bipolar cavity in Models 2 and 3, we were able to successfully simulate a
jet-like structure for the star with a disk wind and created the drop and
subsequent increase in brightness of the system. On the other hand, when the
bipolar cavity is not filled, Model 1 replicates the quiescent state of the
system.
