2014/02/17 by Stephen H. Lubow, Zhaohuan Zhu · 12 citations
Chemistry · Physics and Astronomy · #Astro and Planetary Science #Astrophysics and Star Formation Studies #Atomic physics #Azimuth #Buoyancy #Classical mechanics #Computational physics #Mechanics #Molecular Spectroscopy and Structure #Optics #Physics #Resonance (particle physics) #Thermodynamics #Torque #Wavenumber #astro-ph.EP
paper · pdf · doi:10.1088/0004-637x/785/1/32
published in The Astrophysical Journal 785(1), 32 (IOP Publishing) · 29 pages, 6 figures, accepted for publication in the Astrophysical Journal
arxiv created 2014/02/17 · openalex publication_date 2014/03/21 · arxiv updated 2015/06/18 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Zhu et al. found in three-dimensional shearing box simulations a new form of planet–disk interaction that they attributed to a vertical buoyancy resonance in the disk. We describe an analytic linear model for this interaction. We adopt a simplified model involving azimuthal forcing that produces the resonance and permits an analytic description of its structure. We derive an analytic expression for the buoyancy torque and show that the vertical torque distribution agrees well with the results of the Athena simulations and a Fourier method for linear numerical calculations carried out with the same forcing. The buoyancy resonance differs from the classic Lindblad and corotation resonances in that the resonance lies along tilted planes. Its width depends on damping effects and is independent of the gas sound speed. The resonance does not excite propagating waves. At a given large azimuthal wavenumber k y > h −1 (for disk thickness h ), the buoyancy resonance exerts a torque over a region that lies radially closer to the corotation radius than the Lindblad resonance. Because the torque is localized to the region of excitation, it is potentially subject to the effects of nonlinear saturation. In addition, the torque can be reduced by the effects of radiative heat transfer between the resonant region and its surroundings. For each azimuthal wavenumber, the resonance establishes a large scale density wave pattern in a plane within the disk.