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We present a multi-wavelength analysis of two flare-related jets on November13, 2014, using data from SDO/AIA, RHESSI, Hinode/XRT, and IRIS. Unlike mostcoronal jets where hard X-ray (HXR) emissions are usually observed near the jetbase, in these events HXR emissions are found at several locations, includingin the corona. We carry out the first differential emission measure (DEM)analysis that combines both AIA (and XRT when available) bandpass filter dataand RHESSI HXR measurements for coronal jets, and obtain self-consistentresults across a wide temperature range and into non-thermal energies. In bothevents, hot plasma first appeared at the jet base, but as the base plasmagradually cooled, hot plasma also appeared near the jet top. Moreover,non-thermal electrons, while only mildly energetic, are found in multiple HXRlocations and contain a large amount of total energy. Particularly, theenergetic electrons that produced the HXR sources at the jet top wereaccelerated near the top location, rather than traveling from a reconnectionsite at the jet base. This means that there was more than one particleacceleration site in each event. Jet velocities are consistent with previousstudies, including upward and downward velocities around ~200 km/s and ~100km/s respectively, and fast outflows of 400-700 km/s. We also examine theenergy partition in the later event, and find that the non-thermal energy inaccelerated electrons is most significant compared to other energy formsconsidered. We discuss the interpretations and provide constraints onmechanisms for coronal jet formation.

Observations of magnetic reconnection and particle acceleration locations in solar coronal jets