Three-dimensional transformation of magnetization direction and magnetic field component at low latitudes based on vertical relationship
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Magnetic field driven instabilities in accretion disks are studied using both local and global techniques. A necessary condition for linear and nonlinear instability is derived for disks with both vertical (poloidal) and toroidal magnetic fields. Explicit examples of instabilities are found by a WKB treatment of the governing eigenvalue problem, and verified numerically. Sufficient conditions for instability are derived within the local approximation. In the limit of vanishing vertical magnetic field, the growth rate of the instability is found to be proportional to the product of the vertical wavenumber and the vertical Alfven velocity. When dissipative processes are taken into account, our results show that magnetic instabilities cannot be triggered in a laminar thin disk
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This paper treats the stability of two superposed gravitating streams rotating about the axis transverse to the horizontal magnetic field. The critical wave number for instability is found to be affected by rotation for propagation perpendicular to the axis about which the system rotates. The critical wave number for instability is not affected by rotation when waves propagate along the axis of rotation. The critical wave number is affected by both the magnetic field and the streaming velocity in both cases. Both the magnetic field and the rotation are stabilizing, while the streaming velocity is destabilizing.
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