On the retention of high-energy protons and nuclei with charges Z or equal to 2 in large solar flares after the process of their acceleration

Details On the retention of high-energy protons and nuclei with charges Z or equal to 2 in large solar flares after the process of their acceleration On the retention of high-energy protons and nuclei with charges Z or equal to 2 in large solar flares after the process of their acceleration

Aug 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985icrc....4..229v&link_type=abstract

In NASA. Goddard Space Flight Center 19th Intern. Cosmic Ray Conf., Vol. 4 p 229-232 (SEE N85-34729 23-92)

Physics

Cosmic Rays, Energy Distribution, High Energy Electrons, Interplanetary Space, Particle Acceleration, Solar Activity Effects, Solar Flares, Solar Protons, Charged Particles, Electromagnetic Radiation, Energy Storage, Particle Emission, Solar Atmosphere, Solar Corpuscular Radiation, Trapped Particles

Scientific paper

Data which suggest that the protons with energies of up to several GeV should be retained on the Sun after the process of their acceleration are presented. The protons are on the average retained for 15 min, irrespectively of the solar flare heliolatitude and of the accelerated particle energy ranging from 100 MeV to several GeV. It is suggested that the particles are retained in a magnetic trap formed in a solar active region. No Z or = 2 nuclei of solar origin during large solar flares. The absence of the 500 MeV/nucleon nuclei with Z or = 2 may be due to their retention in the magnetic trap which also retains the high-energy protons. During the trapping time the approx. 500 MeV/nucleon nuclei with Z or = 2 may escape due to nuclear interactions and ionization loss.

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