Determining the CME Morphological and Kinematic Evolution Using Multi-Viewpoint Observations and Rigorous Uncertainty Analysis.

Coronal mass ejections (CMEs) are large-scale phenomena that originate in the Sun and carry plasma and magnetic field into the interplanetary space. They are responsible for the space weather and for this reason studying their initiation and evolution is crucial. In this study we focus on their 3D morphological evolution and kinematics from their source region near the Sun all the way to the outer corona using multi-viewpoint observations in the EUV and white light. We use AIA/ SDO and EUVI/ STEREO data for the early stages of their evolution and as they move higher in the solar atmosphere we switch to COR1 and COR2/ STEREO. A fitting tool that applies the MPFIT minimization IDL routine and combines multi-viewpoint observations with the Graduated Cylindrical Shell model (GCS model) and spheroid shock point clouds in order to obtain the best values of the geometric parameters of each model along with their uncertainties is used to track the CMEs. The evolution of the propagation direction and size of CMEs along with their uncertainties will be analyzed and presented.