The starting conditions for an optically small solar gamma ray flare

Details The starting conditions for an optically small solar gamma ray flare The starting conditions for an optically small solar gamma ray flare

Aug 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985icrc....4...82s&link_type=abstract

In NASA. Goddard Space Flight Center 19th Intern. Cosmic Ray Conf., Vol. 4 p 82-85 (SEE N85-34729 23-92)

Physics

Gamma Rays, Particle Acceleration, Particle Production, Solar Corona, Solar Flares, Solar Protons, Magnetohydrodynamics, Shock Waves, Solar Magnetic Field, Trapped Particles

Scientific paper

It is suggested that optically small gamma-ray flares result from gradual pre-flare acceleration of protons over approximately 1,000 s by a series of magnetohydrodynamic shocks in the low corona. A fraction of the accelerated protons are trapped in the corona where they form a seed population for future acceleration. If the shock acceleration is sufficiently rapid proton energies may exceed the gamma-ray production threshold and trigger gamma-ray emission. This occurs without the total flare energy being necessarily large. Magnetic field geometry is an important parameter.

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