Detecting Spectroscopic Signatures of Magnetic Reconnection Along the Boundary of Coronal Holes

Magnetic reconnection is an essential release mechanism of energy proposed for the highly variable solar wind and plays a direct role in leading to many astrophysical phenomena such as space weather events. Reconnection between open and closed magnetic field lines (i.e. along the boundary of coronal holes) releases coronal loop plasma into the heliosphere as the reconfiguration of the magnetic field accelerates plasma along two reconnection beams. In this investigation we will look for spectral signatures of reconnection occurring along the edges of coronal holes using observations from the EUV Imaging Spectrometer (EIS) onboard Hinode. We will use a novel direct observational method, which we have developed, for detecting magnetic reconnection in the solar atmosphere. Furthermore we will provide a constraint on the energetics at which reconnection occurs. Our preliminary results indicates the presence of spectral lines due to a magnetic reconnection event. Moreover, our preliminary diagnostics indicates that the amount of stray light contamination for the EIS instrument is greater than previously measured.