Solar coronal jets are archetypal examples of reconnection in astrophysical plasmas. Their frequency, simple topology, size and duration make them ideal targets for detailed multiwavelength, multi-instrument analysis. The Interface Region Imaging Spectrograph (IRIS) has the spatial resolution and spectral coverage to observe jet plasma surrounding the reconnection region in unprecedented detail. Using simultaneous IRIS, EIS, XRT, SOT, and AIA observations, we will obtain photospheric magnetic field structure, velocity, density, and non-thermal line widths in order to follow the evolution, coronal plasma dynamics, and energetics of the jet. We will use observations of jets by IRIS, Hinode and SDO to address these goals:
1) Identify the structure and dynamics of the acceleration region in coronal jets. 2) Identify the mechanism for supplying plasma to and accelerating the jet. |
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