Extends magnetogravity polarization formalism to arbitrary magnetic field geometries, revealing avoided crossings and mode conversion below a local field threshold.
Differential rotation and magnetic fields in stellar interiors
4 Pith papers cite this work. Polarity classification is still indexing.
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abstract
The processes contributing to the evolution of an initially weak magnetic field in a differentially rotating star are reviewed. These include rotational smoothing (akin to convective expulsion) and a list of about 5 instabilities, among them magnetorotational instability, byoyancy instability, and pinch-type instabilities. The important effects of thermal and magnetic diffusion on these instabilities are analyzed in some detail. The first instability to set in is a pinch-type instability. It becomes important in modifying the field configuration before magnetic buoyancy-driven instabilities set in. The evolution of an initially strong field remains a more open question, including the old problem whether dynamically stable magnetic equilibria exist in stars.
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UNVERDICTED 4representative citing papers
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