CME Evolution in the Solar Corona

This thesis project aims to investigate how CMEs evolve in the lower corona (rotation, deflection, and expansion) and quantify how this evolution depends on the magnetic structure of the CME (e.g., twist, helicity), the instability responsible for the CME eruption and the properties of the source active regions. The project will combine state-of-the-art time-dependent magnetofrictional modelling and an extensive set of remote-sensing coronal observations. These include Extreme Ultraviolet (=EUV) and coronagraph data from instruments like LASCO aboard of SOHO (= Solar and Heliospheric Observatory), COR1 from STEREO (=Solar Terrestrial Relations Observatory) as well as AIA on SDO (=Solar Dynamics Observatory) and, if available, from Solar Orbiter white-light and EUV instruments.