Aims. Recent observations by the Atacama Large Millimeter/submillimeter Array (ALMA) of
disks around young stars revealed distinct asymmetries in the dust continuum emission. In …

We perform local, vertically stratified shearing-box MHD simulations of protoplanetary disks
(PPDs) at a fiducial radius of 1 AU that take into account the effects of both Ohmic resistivity …

Laboratory experiments indicate that direct growth of silicate grains via mutual collisions can
only produce particles up to roughly millimeters in size. On the other hand, recent …

Rapid orbital drift of macroscopic dust particles is one of the major obstacles to planetesimal
formation in protoplanetary disks. We re-examine this problem by considering the porosity …

ABSTRACT A global picture of the evolution of protoplanetary disks (PPDs) is key to
understanding almost every aspect of planet formation, where standard α-disk models have …

Aims. We investigate the evolution of protoplanetary discs (PPDs) with magnetically driven
disc winds and viscous heating. Methods. We considered an initially massive disc with~ 0.1 …

Planets appear to form in environments shaped by the gas flowing through protostellar disks
to the central young stars. The flows in turn are governed by orbital angular momentum …

Context. The formation of planetesimals is often accredited to the collisional sticking of dust
grains. The exact process is unknown, as collisions between larger aggregates tend to lead …

We investigate gas accretion flow onto a circumplanetary disk from a protoplanetary disk in
detail by using high-resolution three-dimensional nested-grid hydrodynamic simulations, in …

Context. The transition between magnetorotational instability (MRI)-active and magnetically
dead regions corresponds to a sharp change in the disk turbulence level, where pressure …