Protoplanetary disks are quasi-steady structures whose evolution and dispersal determine
the environment for planet formation. I review the theory of protoplanetary disk evolution and …

Planets are built from planetesimals: solids larger than a kilometer that grow by colliding in
pairs. Planetesimals themselves are unlikely to form by two-body collisions alone; …

Context. The global size and spatial distribution of dust is an important ingredient in the
structure and evolution of protoplanetary disks and in the formation of larger bodies, such as …

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 …

Multilayer graphene is an exceptional anisotropic material due to its layered structure
composed of two-dimensional carbon lattices. Although the intrinsic mechanical properties …

Context. The planet-forming region of protoplanetary disks is cold, dense, and therefore
weakly ionized. For this reason, magnetohydrodynamic (MHD) turbulence is thought to be …

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 …

The gas dynamics of weakly ionized protoplanetary disks (PPDs) are largely governed by
the coupling between gas and magnetic fields, described by three non-ideal …

Protoplanetary discs are poorly ionised due to their low temperatures and high column
densities and are therefore subject to three “non-ideal” magnetohydrodynamic (MHD) …