Astronomy and Astrophysics – Astronomy
Scientific paper
Aug 1986
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986esasp.251..101k&link_type=abstract
In ESA Proceedings of the Joint Varenna-Abastumani International School and Workshop on Plasma Astrophysics p 101-104 (SEE N87-
Astronomy and Astrophysics
Astronomy
6
Gamma Ray Astronomy, Helium, Ion Beams, Solar Flares, Solar Magnetic Field, Solar Spectra, Spectrum Analysis, X Ray Astronomy
Scientific paper
Solar energetic particles, X- and γ-ray observations show that during a solar flare both heating of bulk of particles and acceleration of some fraction of them take place. The characteristic proton energy is shown to be about 400 keV. In impulsive flares the acceleration time for protons with energy ≅30 MeV is ⪉2 s. For these flares the parameters of acceleration region are: size L = (1 - 5)×108cm, density n = 1011 - 1013cm-3, magnetic field B = 300 - 2000 Gs. The energy contained in the accelerated (⪆400 keV) ions changes from flare to flare: it is very small in 3He-rich flares and (almost) reaches by the order of magnitude the thermal and magnetic energy of plasma in most powerful impulsive flares. In gradual flares the acceleration mechanism may operate at lower densities (n ≡ 109cm-3) and accelerate ions at longer time scale (≡10 min).
Kocharov Leon G.
Kovaltsov Gennadi A.
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