  Magnetic fields significantly influence the evolution of protoplanetary disks
and the formation of planets, following the predictions of numerous
magnetohydrodynamic (MHD) simulations. However, these predictions are yet
observationally unconstrained. To validate the predictions on the influence of
magnetic fields on protoplanetary disks, we apply 3D radiative transfer
simulations of the polarized emission of aligned aspherical dust grains that
directly link 3D global non-ideal MHD simulations to ALMA observations. Our
simulations show that it is feasible to observe the predicted toroidal
large-scale magnetic field structures, not only in the ideal observations but
also with high-angular resolution ALMA observations. Our results show further
that high angular resolution observations by ALMA are able to identify vortices
embedded in outer magnetized disk regions.
