Alejandro Lara1, Andrea Borgazzi2
1Instituto de
Geofisica, Universidad Nacional Autonoma de Mexico
2Instituto Nacional de Pesquisas Espaciais,
Brazil
Coronal mass ejections (CMEs) are large scale structures of plasma and magnetic field expelled from the Sun to the interplanetary medium and generally observed in white light coronagraphs. During their travel in the inner heliosphere, these 'interplanetary coronal mass ejections' (ICMEs), suffer acceleration due to the interaction with the ambient solar wind. This process can be understood as a transference of momentum between the ICME and the ambient solar wind. In this work, we approach the problem from the point of view of the fluid dynamics and consider the ICMEs-solar wind system as two interacting fluids. We have determined exact solutions of the ICME velocity as a function of time and distance and by comparing our analytic results with observed interplanetary Type II bursts, we suggest values for the viscosity and drag coefficient parameters in this system.