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HD 163296 is a Herbig Ae star that underwent a dramatic $\sim$0.8 magnitudedrop in brightness in the V photometric band in 2001 and a brightening in thenear-IR in 2002. Because the star possesses Herbig-Haro objects travelling inoutflowing bipolar jets, it was suggested that the drop in brightness was dueto a clump of dust entrained in a disk wind, blocking the line-on-sight towardthe star. In order to quantify this hypothesis, we investigated the brightnessdrop at visible wavelengths and the brightening at near-IR wavelengths of HD163296 using the Monte Carlo Radiative Transfer Code, HOCHUNK3D. We createdthree models to understand the events. Model 1 describes the quiescent state ofthe system. Model 2 describes the change in structure that led to the drop inbrightness in 2001. Model 3 describes the structure needed to produce theobserved 2002 brightening of the near-IR wavelengths. Models 2 and 3 utilize acombination of a disk wind and central bipolar flow. By introducing a filledbipolar cavity in Models 2 and 3, we were able to successfully simulate ajet-like structure for the star with a disk wind and created the drop andsubsequent increase in brightness of the system. On the other hand, when thebipolar cavity is not filled, Model 1 replicates the quiescent state of thesystem.

astrophysical journal/the astrophysical journal

Variability of Disk Emission in Pre-Main Sequence and related Stars. V.  Occultation Events from the innermost disk region of the Herbig Ae Star HD  163296