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Gamma-Ray Lines from Solar Flares

Published online by Cambridge University Press:  14 August 2015

R. Ramaty  and
R. E. Lingenfelter
R. Ramaty
Affiliation:
Laboratory for High Energy Astrophysics, NASA-Goddard Space Flight Center, Greenbelt, Md., U.S.A.
R. E. Lingenfelter
Affiliation:
Dept. of Planetary and Space Science, University of California, Los Angeles, Calif., U.S.A.

Abstract

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We have treated in detail the theory of gamma-ray line production in solar flares. The strongest line, both predicted theoretically and detected observationally at 2.2 MeV, is due to neutron capture by protons in the photosphere. The neutrons are produced in nuclear reactions of flare accelerated particles which also produce positrons and prompt nuclear gamma rays. From the comparison of the observed and calculated intensities of the lines at 4.4 or 6.1 MeV to that of the 2.2 MeV line it is possible to deduce the spectrum of accelerated nuclei in the flare region; and from the absolute intensities of these lines it is possible to obtain the total number of accelerated nuclei at the Sun. The study of the 2.2 MeV line also gives information on the amount of He3 in the photosphere. The study of the line at 0.51 MeV resulting from positron annihilation complements the data obtained from the other lines; in addition it gives information on the temperature and density in the annihilation region and on the anisotropy of the accelerated electron beam which produces continuum gamma rays at energies greater than about 1 MeV.

Type
Part 3: Solar Flares
Information
Symposium - International Astronomical Union , Volume 68: Solar X, Gamma, and EUV Radiation , 1975 , pp. 363 - 383
Copyright
Copyright © Reidel 1975 

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