Time-dependent 2.2-MeV and 0.5-MeV lines from solar flares

Details Time-dependent 2.2-MeV and 0.5-MeV lines from solar flares Time-dependent 2.2-MeV and 0.5-MeV lines from solar flares

Dec 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975apj...202..532w&link_type=abstract

Astrophysical Journal, vol. 202, Dec. 1, 1975, pt. 1, p. 532-542.

Astronomy and Astrophysics

Astrophysics

13

Gamma Rays, Nuclear Reactions, Solar Flares, Time Dependence, Emission Spectra, Line Spectra, Positrons, Radiant Flux Density, Radioactive Decay

Scientific paper

The time dependences of the 2.2- and 0.51-MeV gamma-ray lines from solar flares are calculated, and the results are compared with observations of the 1972 August 4 and 7 flares. The time lag between the nuclear reactions and the formation of these two lines is caused by capture of the neutrons and subsequent deceleration of the positrons and decay of the radioactive nuclei. Our main results are that the calculation is consistent with the observed rise of the 2.2-MeV line on August 4, and it does not require different time dependences for the accelerated protons and high-energy electrons in the flare region. The above lags can explain the delayed gamma-ray emission observed on August 7. Positrons of energies greater than about 10 MeV could be detected in interplanetary space following large solar flares.

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