On the Formation of Coronal Mass Ejection with Low Final Speed

Abstract

The two limb CMEs considered in this paper differ from the cases of type 1 and type 2 CMEs studied earlier in [1]. At the same time, they noticeably differ from each other in the nature of their formation, which remains not completely clear. It is unusual in the formation of the April 29, 2014 CME that its appearance is associated with the eruption of only a larger part of the magnetic rope. A specific feature of the February 11, 2014 CME is the fact that it already has a very high velocity of motion near the surface of the Sun - about 1300 km/s, which rapidly decreases as it moves away from the Sun. But they are united by the fact that they both have an extremely low final speed of the CME - no more than 350 km / s. The answer to the question of what determines the formation of these slow CMEs (ICMEs for short) is important for further studies of the dynamics and nature of CMEs.