Dust Distributions in Protoplanetary Disks from Disk Winds

I present results from the simulation of dust grain dynamics in a protoplanetary disk. The simulation comprises a time-evolved gas distribution from magnetohydrodynamic simulations, over which dust grains move vertically along magnetic field lines. I find that smaller grain sizes on the order of 0.1-1 μm are strongly influenced by winds and are lifted from the disk, while larger grain sizes settle more on the midplane. I used Monte Carlo radiative transfer simulations of the resulting dust grain distributions to finally produce dust temperatures and simulated observations of the disk. In doing this, I consider how substructures found within the disk determine the appearance of disks observed in scattered light at near-infrared wavelengths.