Solar prominence dynamic model

The possibility of solar prominence formation due to the motion of magnetized plasma particles has been studied. As a result of such motions, chromospheric and coronal plasma can locally condense to density ∼10 11 cm −3 and to appearance of the current of unmagnetized protons to ∼10 12 A, which corresponds to the values typical of prominences. The model calculations of the studied process indicated that plasma is condensed on a neutral magnetic surface in the form of a stable formation with prominence geometric parameters. This process can proceed if the magnetic field octupole harmonic is significant to altitudes of ≥0.1 R Sun and the magnetic field strength continuously decreases. The latter condition corresponds to observational data and is considered a necessary condition for the appearance of a prominence.