2007/11/29 by Alexander S. Silbergleit, Robert V. Wagoner · 1 citation
Physics and Astronomy · #Accretion (finance) #Accretion disc #Angular momentum #Astrophysical Phenomena and Observations #Astrophysics and Star Formation Studies #Instability #Inviscid flow #Magnetorotational instability #Oscillation (cell signaling) #Pulsars and Gravitational Waves Research #Resonance (particle physics) #Rotational symmetry #WKB approximation #astro-ph #gr-qc
paper · pdf · doi:10.1086/588013
published as Astrophysical Journal 680, 1319 (2008) · 16 pages, no figures. Submitted to The Astrophysical Journal
arxiv created 2007/11/29 · openalex publication_date 2008/06/13 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We demonstrate that the corotation resonance affects only some nonaxisymmetric g -mode oscillations of thin accretion disks, since it is located within their capture zones. Using a more general (weaker radial WKB approximation) formulation of the governing equations, such g -modes, treated as perfect fluid perturbations, are shown to formally diverge at the position of the corotation resonance. For the known g -modes with moderate values of the radial mode number and axial mode number (and any vertical mode number), the corotation resonance lies well outside their trapping region (and inside the innermost stable circular orbit), so the observationally relevant modes are unaffected by the resonance. The axisymmetric g -mode has been seen by Reynolds & Miller in a recent inviscid hydrodynamic accretion disk global numerical simulation. We also point out that the g -mode eigenfrequencies approximately obey the harmonic relation σ ∝ m for axial mode numbers | m| ⩾ 1.