Abstract
Magnetic reconnection is a phenomenon where the energy stored in the magnetic field dissipates into plasma heating and acceleration. It can occur on boundaries connecting plasma with dif ferent magnetic field orientations.
In spacecraft observations, we can identify magnetic reconnection through its exhaust where the plasma on reconnected field lines leaves the reconnection site. We present a statistical study of magnetic reconnection in the solar wind based on data from the WIND spacecraft during the period of 1995{2010.
We track the signatures of the magnetic reconnection exhaust such as a rotation of the magnetic fi eld or acceleration and heating of the plasma. We found dependence of the heating and plasma acceleration inside reconnection exhaust.