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.
Title resolution pending
1 Pith paper cite this work. Polarity classification is still indexing.
1
Pith paper citing it
fields
astro-ph.SR 1years
2026 1verdicts
UNVERDICTED 1representative citing papers
citing papers explorer
-
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.