On the relation between solar-flare gamma-ray emission and proton escape into interplanetary space

Physics

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Gamma Ray Spectra, Interplanetary Medium, Solar Flares, Solar Protons, Solar Radiation, Space Plasmas, Energetic Particles, Magnetohydrodynamic Stability, Magnetohydrodynamic Waves, Particle Acceleration, Particle Diffusion, Solar Magnetic Field, Solar X-Rays

Scientific paper

It is shown that escaping of solar flare energetic protons into interplanetary space as well as their relation to the flare gamma-ray emission depend on the parameter β = 8πp/B02, where p is the pressure of hot plasma and energetic particles and B0 is the magnetic field in a flaring loop. If β very low 1, the bulk of the energetic protons escape to the loss cone because of diffusion due to small-scale Alfvén-wave turbulence, and precipitate into the footpoints of the flaring loop. The flare then produces intense gamma-ray line emission and a weak flux of high energy protons in interplanetary space. If β > β* ≅ 0.3 - 1.0, then fast eruption of hot plasma and energetic particles out of the flaring loop occurs, this being due to the flute instability or "magnetic-field-plasma" nonequilibrium. The flare then produces a comparatively weak gamma-radiation and rather intense proton fluxes in interplanetary space.

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