2011/09/09 by Oleg N. Kirillov, Frank Stefani
Mathematics · Physics and Astronomy · #Accretion (finance) #Angular momentum #Astro and Planetary Science #Astrophysical Phenomena and Observations #Astrophysics #Astrophysics and Star Formation Studies #Classical mechanics #Differential rotation #Geometry #Gravitational singularity #Instability #Magnetic field #Magnetohydrodynamics #Magnetorotational instability #Mathematics #Mechanics #Physics #Rotation (mathematics) #Turbulence #astro-ph.SR #math-ph #math.MP #nlin.PS #physics.flu-dyn
paper · pdf · doi:10.1007/s10440-012-9689-z
published as Acta Applicandae Mathematicae, 2012, 120(1), 177-198 · 25 pages, 10 figures. A tutorial paper. Invited talk at SPT 2011, Symmetry and Perturbation Theory, 5 - 12 June 2011, Otranto near Lecce (Italy)
arxiv created 2011/09/09 · openalex publication_date 2012/02/15 · arxiv updated 2012/07/13 · openalex created_date 2021/02/01 · openalex updated_date 2026/07/23
The magnetorotational instability (MRI) triggers turbulence and enables outward transport of angular momentum in hydrodynamically stable rotating shear flows, e.g., in accretion disks. What laws of differential rotation are susceptible to the destabilization by axial, azimuthal, or helical magnetic field? The answer to this question, which is vital for astrophysical and experimental applications, inevitably leads to the study of spectral and geometrical singularities on the instability threshold. The singularities provide a connection between seemingly discontinuous stability criteria and thus explain several paradoxes in the theory of MRI that were poorly understood since the 1950s.