Abstract
Magnetic reconnection is a phenomenon where the energy stored in magnetic field dissipates into heating and particle acceleration. It can occur on boundaries connecting plasma with different magnetic field topology.
We can frequently find magnetic reconnection in ICME sheaths, where plasma is compressed and different plasma topologies encounter each other. In these regions we can recognize magnetic reconnection by number of plasma signatures such as temperature enhancement, or changes in magnetic field and bulk flow direction.
A brief introduction into Interplanetary Coronal Mass Ejection (ICME), magnetic reconnection and its properties are presented and short statistics on shear angle dependence are provided. We have found dependence of temperature enhancement inside reconnection exhaust on shear angle.
We have also obtained dependence of reconnection outflow speed on shear angle.