Other
Scientific paper
Mar 1983
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983apj...266..370h&link_type=abstract
Astrophysical Journal, Part 1, vol. 266, Mar. 1, 1983, p. 370-372.
Other
11
Helium Isotopes, Particle Acceleration, Radiation Pressure, Resonance Lines, Solar Cosmic Rays, Solar Flares, Solar Corona, Thermal Energy
Scientific paper
The enrichment of He-3 in solar flare particles is explained by the radiation pressure of helium resonance lines. Since the resonance level of He-3 is isotropically shifted, the scattering of a strong resonance line emitted from He-4 is possible if the line is Doppler shifted in the course of acceleration. The chromospheric emission of He Ly-Alpha can accelerate He-3 to energies appreciably higher than the thermal energy, so that He-3 takes an advantage in later acceleration by different mechanisms. The acceleration site is of low density, in order to get rid of charge changing collisions in the course of acceleration. Coronal cool regions as suggested by the presence of He(+) in solar energetic particles are favorable for the acceleration site. The mechanism proposed works selectively for He-3 with weaker constraints than other mechanisms thus far proposed.
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