| Abstract |
Planet formation takes place in gas-rich protoplanetary disks (PPDs) orbiting newly
born stars. The internal density and flow structures of PPDs, as well as their
long-term evolution, play a crucial role in almost all stages of planet formation,
yet they are far from being well understood largely due to the complex interplay
among various microphysical processes. I will review the basic physical processes in
PPDs that govern disk structure and evolution, highlighting the fundamental role of
disk ionization and magnetic fields, described by non-ideal magnetohydrodynamic
(MHD) effects. Incorporating these processes, I will present global simulations of
PPDs aiming to incorporate most realistic disk microphysics, which demonstrate
unusual flow structures with major implications on planet formation. The results
will also be discussed in the context of current and future observations.
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