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The present work illustrates the potential of a new diagnostic technique thatallows the measurement of the coronal magnetic field strength in solar activeregions utilizing a handful of bright \ion[Fe x] and \ion[Fe xi] lines commonlyobserved by the Hinode/EIS high-resolution spectrometer. The importance of thisnew diagnostic technique lies in two basic facts: 1) the coronal magnetic fieldis probably the most important quantity in coronal physics, as it is at theheart of the processes regulating Space Weather and the properties of the solarcorona, and 2) this technique can be applied to the existing EIS archivespanning from 2007 to 2020, including more than one full solar cycle andcovering a large number of active regions, flares, and even coronal massejections. This new diagnostic technique opens the door to a whole new field ofstudies, complementing the magnetic field measurements from the upcoming DKISTand UCoMP ground based observatories, and extending our reach to active regionsobserved on the disk and until now only sampled by radio measurements. In thiswork we present a few examples of the application of this technique to EISobservations taken at different times during the EIS mission, discuss itscurrent limitations and the steps to improve its accuracy. We also present alist of EIS observing sequences whose data include all the lines necessary forthe application of this diagnostic technique, to help the solar communitynavigate the immense set of EIS data and to find observations suitable tomeasure the coronal magnetic field.

Hinode/EIS measurements of active region magnetic fields