Speaker
Description
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 observations, we will show that buoyancy spirals can produce observable kinematic signatures. One of the main characteristics of buoyancy spirals is their tightly-wound morphology (i.e., a small pitch angle compared with Lindblad spirals). The strength and observability of buoyancy spirals depend sensitively on the disk thermodynamics. This highlights the importance of using more realistic thermodynamics in hydrodynamic simulations.
