  Global numerical simulations of protoplanetary disk formation and evolution
were conducted in thin-disk limit, where the model included magnetically
layered disk structure, a self-consistent treatment for the infall from cloud
core as well as the smallest possible inner computational boundary. We compared
the evolution of a layered disk with a fully magnetically active disk. We also
studied how the evolution depends on the parameters of the layered disk model -
the MRI triggering temperature and active layer thickness - as well as the mass
of the prestellar cloud core.
  With the canonical values of parameters a dead zone formed within the inner
$\approx$ 15 au region of the magnetically layered disk. The dead zone was not
a uniform structure and long-lived, axisymmetric, gaseous rings ubiquitously
formed within this region due to the action of viscous torques. The rings
showed a remarkable contrast in the disk environment as compared to a fully
magnetically active disk and were characterized by high surface density and low
effective viscosity. Multiple gaseous rings could form simultaneously in the
dead zone region which were highly dynamical and showed complex, time-dependent
behavior such as inward migration, vortices, gravitational instability and
large-scale spiral waves. An increase in MRI triggering temperature had only
marginal effects, while changes in active layer thickness as well as the
initial cloud core mass had significant effects on the structure and evolution
of the inner disk. Dust with large fragmentation barrier could be trapped in
the rings, which may play a key role in planet formation.
