Physics
Scientific paper
Sep 1985
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985soph...99..313z&link_type=abstract
Solar Physics (ISSN 0038-0938), vol. 99, Sept. 1985, p. 313-321.
Physics
21
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.
Stepanov Alexander V.
Zaitsev Valerii V.
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