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Impulsive solar energetic-particle (SEP) events were first distinguished asthe streaming electrons that produce type III radio bursts as distinct fromshock-induced type II bursts. They were then observed as thesurprisingly-enhanced 3He-rich SEP events, which were also found to haveelement enhancements rising smoothly with the mass-to-charge ratio A/Q throughthe elements, even up to Pb. These impulsive SEPs have been found to originateduring magnetic reconnection in solar jets where open magnetic field linesallow energetic particles to escape. In contrast, impulsive solar flares areproduced when similar reconnection involves closed field lines where energeticions are trapped on closed loops and dissipate their energy as X-rays,{\gamma}-rays, and heat. Abundance enhancements that are power-laws in A/Q canbe used to determine Q values and hence the coronal source temperature in theevents. Results show no evidence of heating, implying reconnection and ionacceleration occur early, rapidly, and at low density. Proton and He excessesthat contribute their own power-law may identify events with reacceleration ofSEPs by shock waves driven by accompanying fast, narrow coronal mass ejections(CMEs) in many of the stronger jets.

Element Abundances in Impulsive Solar Energetic-Particle Events