Gravitational coupling between protoplanetary disks and embedded planets is an old problem ascending to the seminal studies of Goldreich & Tremaine (1980) and Lin & Papaloizou (1979). It is widely recognized as playing a key role in many areas of exoplanetary science: determination of the planetary architectures, disk evolution, planetary accretion, and so on. In this talk I will describe...
Understanding the origins and dynamics of massive planets during the planet-formation process is essential to understanding how the structures of individual planetary systems came to be. Massive planets have the ability to open gaps in their host disk, and the radial movements of these gap-opening planets is typically referred to as type II migration. In the classical view, a protoplanetary...
Recent ALMA observations revealed concentric annular structures in several young, class-II objects. Some have been modeled numerically with a single embedded planet assuming a locally isothermal equation of state, a method often used in the irradiation-dominated outer disk regions. We compare locally isothermal and radiative disks similar to HD 163296 and AS 209 with embedded planets and
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Spiral waves are one of the most fundamental outcomes of planet-disk interaction. In addition to the well-known Lindblad resonance, buoyancy resonance, which occurs when the vertical buoyancy frequency of disk gas matches with an integer multiple of the planet's orbital frequency, can excite spiral waves. Based on three-dimensional global hydrodynamic simulations and synthetic ALMA line...
The classic view of a viscous disk, where viscosity is generated by strong turbulence driven by the magneto rotational instability, is challenged by modern magneto-hydrodynamic simulations. Disks are probably much less viscous than previously thought. Nevertheless, disks cannot be in-viscid, a minimum viscosity is set for example by the so-called vertical shear instability (VSI). In addition,...
Giant planet migration (a.k.a. Type-II migration) should occur with a migration speed proportional to the disk's viscosity. This has been verified for alpha-disks with alpha>1.e-4 (Robert et al., 2018). But what happens in disks with vanishing viscosity? Does Type-II migration stalls? A variety of behaviors have been observed in the literature for migration in low-viscosity disks. Migration...
Recently, young planets with masses around $10\,M_\text{Jupiter}$ which are still embedded in a disk have been observed, e.g. in the PDS 70 system. At this mass range, the planet-disk interaction is non-linear and the planets are attributed with having carved the observed gap into their parent disk. One possible scenario for the formation of large gaps is outward migration in 2:1 mean motion...
