Analysis of Deformation and Erosion during CME Evolution

Magnetised coronal mass ejections (CMEs) are quite substantially deformed during their journey form the Sun to Earth. Moreover, interaction of internal magnetic field with ambient solar wind can cause deflection and erosion flux. We here analyse axisymmetric (2.5D) MHD simulations normal inverse CME, i.e., opposite or same polarity as background wind, attempt quantify different forces that operate on CMEs evolution. By analysing forces, it was found an increase density results in a stronger plasma pressure gradient sheath decelerates cloud more. This turn leads between centre separatrix, causing further deceleration. Regardless polarity, current sheet forms our model rear CME closed lines helmet streamer, being stripped from cloud. It is also slow experience amount erosion, regardless density. initial velocity increases, so does influence erosion. increasing speed higher overall due reconnection. For CMEs, not away but added cloud, leading about twice much flux at 1 AU than