A key stage in planet formation is the evolution of a gaseous and magnetized solar nebula.
However, the lifetime of the nebular magnetic field and nebula are poorly constrained. We …

This review examines recent theoretical developments in our understanding of turbulence in
cold, non-magnetically active, planetesimal-forming regions of protoplanetary disks that we …

We perform streaming-instability simulations at Hill density and beyond to demonstrate that
planetesimal formation is not completed when pebble accumulations exceed the local Hill …

Stably stratified Taylor–Couette flow has attracted much attention due to its relevance as a
canonical example of the interplay among rotation, stable stratification, shear and container …

Theoretical models of protoplanetary discs have shown the vertical shear instability (VSI) to
be a prime candidate to explain turbulence in the dead zone of the disc. However …

The streaming instability is a leading candidate mechanism to explain the formation of
planetesimals. However, the role of this instability in the driving of turbulence in …

Disk vortices have been heralded as promising routes for planet formation due to their ability
to trap significant amounts of pebbles. While the gas motions and trapping properties of two …

Context. Hydrodynamic, non-magnetic instabilities can provide turbulent stress in the
regions of protoplanetary discs, where the magneto-rotational instability can not develop …

Turbulence has a profound impact on the evolution of gas and dust in protoplanetary disks
(PPDs), from driving the collisions and the diffusion of dust grains, to the concentration of …

Theoretical models of protoplanetary disks including stellar irradiation often show a
spontaneous amplification of scale height perturbations, produced by the enhanced …