CME stimulated by eruptive prominence

A model of CME arising due to drift motion in the corona in the presence of an eruptive prominence is presented. Magnetic field configuration is in accordance with a model of inverse polarity. In a region where a magnetic pressure of the filament magnetic field is greater than a gas pressure, plasma motion can be assumed as a drift motion. Its characteristic is such that the further one gets from the filament, the higher is drift velocity of a plasma. That sort of motion leads to a rarefaction of plasma and formation of a cavity around the filament. But a current strength in eruptive prominences estimated from observations is such that the region b is less than 1 has a limited size. Near the boundary b = 1 plasma deceleration is occurred and as a result of it coronal density is increasing. Plasma condensation near the surface b = 1 leads to formation of a dense envelope which can be collated with an outer loop of CME. Two dimensional numerical MHD simulation displays a process of cavity and loop formation. If a current is large enough, two compact regions of compressed dense matter arise at both sides of the rising filament and two narrow jets are developed. This scenario, perhaps, corresponds to CMEs in which a top of the loop is faint or it is absent at all.