Stretching of the toroidal field and generation of magnetosonic waves in differentially rotating plasma

Abstract

We evaluate the generation of magnetosonic waves in differentially rotating magnetized plasma. Differential rotation leads to an increase of the azimuthal field by winding up the poloidal field lines into the toroidal field lines. An amplification of weak seed perturbations is considered in this time-dependent background state. It is shown that seed perturbations can be amplified by several orders of magnitude in a differentially rotating flow. The only necessary condition for this amplification is the presence of a non-vanishing component of the magnetic field in the direction of the angular velocity gradient.

arXiv comment5 pages, 5 figures

References in corpus (9)

• Global Magnetohydrodynamical Simulations of Accretion Tori
• The Stability of Magnetized Rotating Plasmas with Superthermal Fields
• Waves and Instabilities in Accretion Disks: MHD Spectroscopic Analysis
• The Magnetohydrodynamics of Convection-Dominated Accretion Flows
• Two-Dimensional Hydrodynamic Simulations of Convection in Radiation-Dominated Accretion Disks
• Magneto-rotational overstability in accretion disks
• Hydromagnetic Instability in Differentially Rotating Flows
• Compressibility and local instabilities of differentially rotating magnetized gas
• Convective magneto-rotational instabilities in accretion disks

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