In radiatively inefficient, laminar protoplanetary discs, embedded planets can excite a
buoyancy response as gas gets deflected vertically near the planet. This results in vertical …

The key difficulty faced by 2D models for planet–disc interaction is in appropriately
accounting for the impact of the disc's vertical structure on the dynamics. 3D effects are often …

Protoplanets may be born into dust-rich environments if planetesimals formed through
streaming or gravitational instabilities, or if the protoplanetary disc is undergoing mass-loss …

We present two-dimensional inviscid hydrodynamic simulations of a protoplanetary disk with
an embedded planet, emphasizing the evolution of potential vorticity (the ratio of vorticity to …

In the innermost regions of protoplanerary discs, the solid-to-gas ratio can be increased
considerably by a number of processes, including photoevaporative and particle drift …

Context. It is well known that partial and deep gap opening depends on a disc's viscosity;
however, damping formulas for orbital eccentricities have only been derived at high …

Context. Several observations of protoplanetary disks reveal non-axisymmetric features,
which are often interpreted as vortices. Numerical modeling has repeatedly shown that gap …

Context. While planets in the solar system only have a low inclination with respect to the
ecliptic there is mounting evidence that in extrasolar systems the inclination can be very …

Low-mass planets migrating inwards in laminar protoplanetary disks (PPDs) experience a
dynamical corotation torque, which is expected to slow down migration to a stall. However …

Young planets embedded in protoplanetary discs (PPDs) excite spiral density waves, which
propagate shock and deposit angular momentum in the disc. This results in gap opening …