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Presentation #302.03 in the session From the Photosphere to the Corona, Solar Eruptive Events.
Understanding the structure of currents in the corona has been a long standing goal of solar physics. Coronal currents provide the energy for solar eruptions and are the origin of the magnetic fields that form flux-ropes and sites of reconnection. We present a new technique for determining the fingerprints of coronal currents in photospheric vector magnetograms. We discuss the implications of this method for understanding flares, flux emergence, forces, helicity, free energy, and coronal modeling.