The formation of planetesimals is expected to occur via particle-gas instabilities that
concentrate dust into self-gravitating clumps,–. Triggering these instabilities requires the …

We study the torque on low-mass planets embedded in protoplanetary discs in the two-
dimensional approximation, incorporating non-isothermal effects. We couple linear …

We perform numerical simulations of a disc–planet system using various grid-based and
smoothed particle hydrodynamics (SPH) codes. The tests are run for a simple setup where …

Radiation transport plays a crucial role in star formation models, as certain questions within
this field cannot be accurately addressed without taking it into account. Given the high …

We present the results of numerical simulations of protostellar accretion disks that are
perturbed by a protoplanetary companion that has a much smaller mass than the central …

We study the structure and dynamics of the gap created by a protoplanet in an accretion
disc. The hydrodynamic equations for a flat, two-dimensional, non-self-gravitating …

Interstellar magnetic fields play certainly a distinct role in star formation and in galactic
molecular disks. These magnetic fields are, however, also a key ingredient for accretion …

We investigate the gravitational interaction of a Jovian-mass protoplanet with a gaseous disc
with aspect ratio and kinematic viscosity expected for the protoplanetary disc from which it …

A large fraction of giant planets have gaseous envelopes that are limited to about 10% of
their total mass budget. Such planets are present in the solar system (Uranus, Neptune) and …

Aims. We investigate the effect of including a proper energy balance on the interaction of a
low-mass planet with a protoplanetary disk. Methods. We use a three-dimensional version of …