Magnetic filaments in the solar convection zone form in two stages: a kinematic frozen-in phase at convective cell boundaries followed by a dynamic phase where magnetic pressure alters the flow until kinetic and magnetic energy densities become comparable.
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Two stages of magnetic filament formation in the solar convective zone
Magnetic filaments in the solar convection zone form in two stages: a kinematic frozen-in phase at convective cell boundaries followed by a dynamic phase where magnetic pressure alters the flow until kinetic and magnetic energy densities become comparable.