A controlled multiscale RMHD expansion in arbitrary magnetic geometry yields new geometry-driven turbulent heating and cross-field transport channels that can dominate standard reflection in structured coronal regions.
Differential rotation and magnetic fields in stellar interiors
5 Pith papers cite this work, alongside 80 external citations. Polarity classification is still indexing.
5
Pith papers citing it
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external citations · Pith
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.
years
2026 5representative citing papers
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