Speaker: Satoshi Okuzumi<\/p>\n\n\n\n
The thermal structure of protoplanetary disks determines when and where planets of different compositions form. However, the thermal structure of these disks remains largely uncertain due to two main factors: (1) the existence of strong internal heating sources deep inside the disks is still unknown, and (2) the cooling rate of the disks is influenced by micron-sized dust grains and varies as the grains grow into larger solid bodies. Dust growth can even impact disk heating induced by magnetic fields, as the grains regulate the disks’ electric conductivity by capturing plasmas. All these factors indicate that the temperature structure of the disks evolves as planet formation (dust evolution) progresses. In this presentation, I will discuss our recent efforts to model the coupled evolution of dust and the thermal structure of protoplanetary disks. Specifically, I will highlight the roles played by magnetic fields, disk shadows, and planet-induced spiral shocks in shaping the disks’ temperature distribution.<\/p>\n","protected":false},"excerpt":{"rendered":"