2014/12/15 by Maciek Wielgus, P. Chris Fragile, Ziming Wang +2 · 1 citation
Physics and Astronomy · #Angular momentum #Angular momentum coupling #Astrophysical Phenomena and Observations #Astrophysics and Cosmic Phenomena #Black hole (networking) #Classical mechanics #Dispersion relation #Geometry #Magnetic field #Magnetohydrodynamic drive #Magnetohydrodynamics #Mechanics #Physics #Plasma #Pulsars and Gravitational Waves Research #Quantum mechanics #Rotating black hole #Rotational symmetry #Specific relative angular momentum #Stability (learning theory) #Toroid #Torus #Total angular momentum quantum number #astro-ph.HE
paper · pdf · doi:10.1093/mnras/stu2676
published as MNRAS 447 (4): 3593-3601, 2015 · 9 pages, 11 figures, accepted in MNRAS
arxiv created 2014/12/15 · openalex publication_date 2015/01/24 · arxiv updated 2015/02/12 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We investigate the local stability of strongly magnetized relativistic tori orbiting Kerr black holes, for the case of a purely toroidal magnetic field topology. Our approach encompasses both solving the full dispersion relation numerically and solving a simplified analytic treatment. Both approaches indicate that such tori are subject to an unstable non-axisymmetric magnetorotational mode, regardless of such background properties as the gas-to-magnetic pressure ratio and specific angular momentum distribution. We demonstrate that our modal analysis matches well with what is seen in global, three-dimensional, general relativistic magnetohydrodynamic simulations.