The Structure of Spiral Shocks Excited by Planetary-mass Companions

摘要: Direct imaging observations have revealed spiral structures in protoplanetary disks. Previous studies suggested that planet-induced arms cannot explain some of these patterns, due to the large pitch angle and high contrast observations. We carried out three dimensional (3-D) hydrodynamical simulations study wakes/shocks excited by young planets. find that, with linear theory, does depend on planet mass, which can be explained non-linear density wave theory. A secondary (or even a tertiary) arm, especially for inner arms, is also massive planet. With more disk, larger separation between primary azimuthal direction larger. although outer disk do not exhibit much vertical motion, significant boosts perturbation at atmosphere. Combining models Monte-Carlo radiative transfer calculations, we are considerably prominent synthetic near-IR images using full 3-D than based 2-D assuming hydrostatic equilibrium, indicating need model hydrodynamics. Overall, companion-induced only pinpoint companion's position but provide independent ways (pitch angle, two arms) constrain mass.