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Recent observations by the Atacama Large Millimeter/submillimeter Array(ALMA) of disks around young stars revealed distinct asymmetries in the dustcontinuum emission. In this work we want to study axisymmetric andnon-axisymmetric structures, evocated by the magneto-rotational instability inthe outer regions of protoplanetary disks. We combine the results ofstate-of-the-art numerical simulations with post-processing radiative transfer(RT) to generate synthetic maps and predictions for ALMA. We performednon-ideal global 3D MHD stratified simulations of the dead-zone outer edgeusing the FARGO MHD code PLUTO. The stellar and disk parameters are taken froma parameterized disk model applied for fitting high-angular resolutionmulti-wavelength observations of circumstellar disks. The 2D temperature anddensity profiles are calculated consistently from a given surface densityprofile and Monte-Carlo radiative transfer. The 2D Ohmic resistivity profile iscalculated using a dust chemistry model. The magnetic field is a vertical netflux field. The resulting dust reemission provides the basis for the simulationof observations with ALMA. The fiducial model develops a large gap followed bya jump in surface density located at the dead-zone outer edge. The jump indensity and pressure is strong enough to stop the radial drift of particles. Inaddition, we observe the generation of vortices by the Rossby wave instability(RWI) at the jumps location close to 60 AU. The vortices are steadily generatedand destroyed at a cycle of 40 local orbits. The RT results and simulated ALMAobservations predict the feasibility to observe such large scale structuresappearing in magnetized disks without having a planet.

Gaps, Rings, and Non-Axisymmetric Structures in Protoplanetary Disks - From Simulations to ALMA Observations