Abstract:
Spatially resolved observations of protoplanetary discs have revealed a multitude of substructures. From gaps and cavities, to spiral arms and perturbed kinematics, these observations are highly suggestive of companion-disc interactions from planetary to stellar mass objects. However other mechanisms, such as the gravitational instability (GI) or late-stage infall, may explain some of these structures. Using hydrodynamical simulations and radiative transfer to produce mock observations, we can understand how to distinguish between these scenarios. By directly comparing with observations, I will show how undetected binary companions and late-stage infall may be an important but overlooked source of disc substructures.
