Positron annihilation in solar flares

Details Positron annihilation in solar flares Positron annihilation in solar flares

Aug 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975icrc....5.1656c&link_type=abstract

In: International Cosmic Ray Conference, 14th, Munich, West Germany, August 15-29, 1975, Conference Papers. Volume 5. (A76-26851

Physics

1

Energy Spectra, Particle Production, Positron Annihilation, Positronium, Solar Flares, X Ray Spectra, Charge Exchange, Continuous Radiation, Gamma Rays, High Energy Interactions, Hydrogen Plasma, Particle Energy, Radiative Recombination

Scientific paper

The gamma-ray line at 0.51 MeV originates from the annihilation of positrons. When a fraction of the positrons annihilate from bound states of positronium, the 0.51 MeV line is accompanied by a continuum of 3-gamma annihilation radiation at energies up to 0.51 MeV. We present accurate calculations of the rates of free annihilation and positronium formation in a solar flare plasma, and we also discuss positronium formation by charge exchange. The observability of the 3-gamma annihilation is increased by the inherent delay in the production and slowing down time of the positrons. We conclude that such radiation could be detected at times late in solar gamma-ray events when the continuum and prompt line emissions have essentially disappeared.

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