How Particle Acceleration, Magnetic Loop Transport, and the solar Atmosphere Affect Gamma-ray and Neutron Production
Abstract
Solar flare energetic ions are thought to be accelerated in the corona and propagate down the legs of magnetic loops to the higher density chromosphere and photosphere. Interactions of these particles with the solar atmosphere result in gamma-ray and neutron emission. The observable quantities associated with these emissions depend on the conditions at the flare site relating to both acceleration (e.g., ion spectra, composition and release time history) and transport (e.g., loop length, particle scattering, magnetic field convergence, ambient abundances). We explore these often complex dependences and describe an analysis procedure that takes best advantage of the dependences and results in realistic uncertainties for estimates of flare parameters. The procedure is applied to the OSSE observations of the 1991 June 4 flare. Constraints are placed on the high-energy (>100 MeV nucleon-1) accelerated ion spectrum which would not be possible without the wide range of measurements available for this flare.This work was supported by NASA Grant NNH06AD55I.
- Publication:
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AAS/Solar Physics Division Meeting #37
- Pub Date:
- June 2006
- Bibcode:
- 2006SPD....37.1301M