Abstract
Magnetic reconnection is a phenomenon where the energy stored in the magnetic eld dissipates into heating and plasma acceleration. It can occur on boundaries connecting plasma with different magnetic field directions.
Magnetic reconnections are common processes in ICME sheaths, where plasma is compressed and plasma with different magnetic field direction encounter each other, or at the boundaries of ICME sheaths and magnetic clouds, where the strongest reconnection with the largest shear angle can be found. In this paper, we trace the magnetic reconnection exhaust which was observed by many spacecraft and obtain its parameters which are dependent on the distance from the X-line.
We analyze differences in the structure of the reconnection exhaust, its evolution and direction of propagation. We discuss energetic particle signature of the magnetic reconnection exhaust.