| Abstract |
The thermal structure of protoplanetary disks is crucial for understanding the origin of water on rocky planets and the process of planet formation. In the conventional disk model, the disk is turbulent, and disk heating and gas accretion are triggered by turbulence-induced viscosity. The viscous heating dissipates gravitational energy around the equatorial plane, resulting in a significant temperature increase in the optically thick disk. This heating process is considered to dominate the thermal structure within the inner several AU regions from a central star. However, when taking into account the magnetohydrodynamics which controls disk dynamics, it has been found that the magnetic turbulence is suppressed under the weakly ionized environment of protoplanetary disks. The disk structure of such magnetically accreting laminar disks is not yet fully understood, and many uncertainties remain regarding their temperature structure. In my presentation, I will present the simulation results of magnetohydrodynamics for the inner regions of protoplanetary disks. Additionally, I will discuss the thermal structure of the disks suggested from these simulations, as well as the temporal evolution of the water snowline. |
