Recent spatially-resolved observations of protoplanetary disks revealed a plethora of
substructures, including concentric rings and gaps, inner cavities, misalignments, spiral …

Giant planets embedded in protoplanetary disks (PPDs) can create annulus density gaps
around their orbits in the type-II regime, potentially responsible for the ubiquity of annular …

Besides the spirals induced by the Lindblad resonances, planets can generate a family of
tightly wound spirals through buoyancy resonances. The excitation of buoyancy resonances …

Context. Models of a planet-disk interaction are mainly based on 2D and 3D viscous
hydrodynamic simulations. In such models, accretion is classically prescribed by an α v …

Capture into mean motion resonance (MMR) is an important dynamical mechanism because
it shapes the final architecture of a planetary system. We simulate systems of two or three …

We carried out 3D dust+ gas radiative hydrodynamic simulations of forming planets. We
investigated a parameter grid of a Neptune-mass, a Saturn-mass, a Jupiter-mass, and a five …

The chemical composition of planetary atmospheres has long been thought to store
information regarding where and when a planet accretes its material. Predicting this …

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 …

Low-mass planets migrate in the type-I regime. In the inviscid limit, the contrast between the
vortensity trapped inside the planet's corotating region and the background disc vortensity …

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 …