Abstract
Most regions of protoplanetary disks are magnetorotationally unstable. Only the inner part of the disk, which is the so-called ‘dead zone’, is stabilized by ohmic dissipation. The characteristics of dust grains affect the abundances of charged particles significantly and change the size of the dead zones. The outer radius is typically around 10 AU, but could be zero. The gas, dust grains and magnetic field in protoplanetary disks are closely correlated with each other and thus the evolution of these components should be solved consistently. Especially dust evolution in turbulent disks is an important process in planet formation theory.
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