Hydrodynamic models of dusty protoplanetary disks
Small solids in protoplanetary disks are the building blocks of planets. However, modeling the interaction between small dust (<~1mm) and gaseous disks can be numerically challenging. I will introduce a new conceptual approach to study protoplanetary disks containing small dust particles. I show how one can describe a dusty disk within a purely hydrodynamical, dust-free framework. I will demonstrate this simplified modeling still captures the essential physics in dusty protoplanetary disks, such as particle trapping at pressure maxima and streaming instabilities.