Abstract:
Protoplanetary disks are the birthplaces of planets. However, these disks also embed young planets, making them extremely difficult to detect. Substructures within the disks, especially those observed in millimeter-wavelength dust thermal emissions, such as gaps and rings, have been used to suggest the presence of planets. Nevertheless, planet-disk interactions are not the only mechanisms that can explain these features. Therefore, distinguishing substructures caused by planets from those of other origins is crucial for current planet-hunting efforts and for understanding the planet formation process. In this talk, I will summarize our recent studies of dust dynamics under planet-disk interactions using three-dimensional numerical simulations. Our findings show that incorporating the vertical dimension into planet-disk models reveals a wealth of dynamics, potentially leading to characteristic features in observations.
