Eruption of Prominences

Sometimes filaments that have existed for a long time above the solar surface either demonstrate rapid changes and movements, or disappear from view altogether. Rapidly rising prominences are called eruptive prominences. The general properties of eruptive prominences and their kinematics are considered. In most cases, there is no convincing evidence of the presence of an external source of excitation of the prominence than could lead to an eruption. The cause of prominence eruptions seems to be in properties of the prominence equilibrium, the possibility of developing instabilities. The structure of the coronal magnetic field not only determines the height of the onset of eruption, but also guides the direction of the motion of eruptive prominences.