12-20 July 2017
Asia/Seoul timezone
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BEXCO - Room C(106/107)

[SH125] Comparison of Long Duration Gamma-Ray Flares at the Sun and High-Energy 1-AU Solar Energetic Particles



Primary authors



High-energy and sustained emission from Long Duration Gamma-Ray Flares (LDGRFs), identified with Compton Gamma-Ray Observatory (CGRO), the Solar Maximum Mission (SMM), and now Fermi, has been a challenge to explain. The highest energy emission has generally been attributed to pion production from the interaction of high-energy protons with the ambient matter, suggesting that particle acceleration occurs over large volumes extending high in the corona, either from stochastic acceleration within large coronal loops or from back precipitation from CME-driven shocks. It is possible to test these models by making direct comparisons between the accelerated ion population at the flare derived from the observations of Fermi/LAT and PAMELA measurements of solar energetic particles in the energy range corresponding to the pion-related emission. For nearly a dozen SEP events, we compare the two populations (SEPs in space and the interacting population at the Sun) and discuss the implications in terms of particle acceleration and transport models.