Dust particles in the outer regions of protoplanetary disks can experience moderate levels of turbulence, which can lift them to the disk surface where their icy mantles are exposed to UV photons, altering the chemical composition of the outer disk. By combining hydrodynamical (gas + dust) simulations with a UV radiation field applied in a post-processing step using RADMC3D, we find that a small fraction (~17%) of 100-micron-sized particles are frequently lofted to a height of Z/R = 0.2. At this altitude, their prolonged residence time enables efficient photodissociation of CO and water, potentially erasing their pristine composition. Additionally, particles undergoing radial and vertical turbulent motions can become concentrated in spontaneously formed vortices and zonal flows, leading to local enhancements in the dust-to-gas mass ratio above solar values. These regions of elevated dust density may have significant implications for dust growth and planetesimal formation. We present new results exploring the observational signatures of such particle-loaded pressure bumps and vortices.