Gamma-Ray Observations of Solar-Flare Ion Acceleration

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Solar flares accelerate both electrons and ions to high energies, with comparable energy content in each population, and thus observing the signatures of both populations is crucial to understanding the relevant acceleration processes. Accelerated electrons produce an X-ray signature via bremsstrahlung, while accelerated ions produce a variety of gamma-ray lines through nuclear interactions with the solar atmosphere that reveals not only spectral information of the accelerated population but also abundance information for both the accelerated and ambient populations. A comprehensive study of all RHESSI flares finds proportional acceleration of relativistic electrons above 300 keV and ions above 20 MeV/nucleon, which indicates a common acceleration process. This proportionality also provides constraints for acceleration models. The correlation worsens when considering electrons at lower energies, suggesting that electrons below 300 keV may also be accelerated by other processes. Future balloon-based gamma-ray observations by GRIPS with the unparalleled angular resolution of 12.5 arcseconds will further probe the spatial and angular distributions of both accelerated ions and electrons.

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