Dynamics of Mass Ejections in the Low Corona

The Solar Corona ejects plasma and magnetic field in a large range of scpace-temporal scales. The Solar wind is continuaosly ejected with a mass loss 10^14 Msol/year. Over this flow, spradic eruptions are ejected, from small scale "blobs" with 10^12 g of mass and very low speeds up the large scale "coronal mass ejections" with 10^16 g of mass and speeds ranging from 10^2 to 10^3 km/s. In spite of the large differences, the dynamics of these phenomena has a commun denominator: the interaction of two colisionless plasmas. In this work, we present a statistical study of the dynamics of the coronal ejections considering the drag as the major force. With this assumption we found a very good model for the movement of the ejectas in the corona.