Intimate Relationship Between Plasma Structures and Magnetic Fields in the Solar Atmosphere

The connection between prominences and the magnetic fields of the Sun is shown. The distribution of photospheric magnetic fields determines the location and internal structure of coronal plasma formations. Prominences are elongated along large-scale polarity inversion lines of the photospheric magnetic field (neutral lines). It is shown that the prominence material is concentrated close to the magnetic neutral surface or the surface passing through apices of arches of potential magnetic field lines. The height of prominences above the photosphere depends on the strength of the coronal magnetic field and the magnitude of the electric current flowing in the prominence. There is a maximum height for the stable equilibrium of prominences in a given magnetic field, determined by the scale of the field. Peculiarities of the fine structure of filaments, such as barbs and transversal segments, are also associated with the smaller-scale distribution of photospheric magnetic fields near the polarity inversion line. Coronal streamers and polar plumes are more related to the structure of the global magnetic field of the Sun and reflect its evolution during solar cycles.