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- W7524203 abstract "As we note in Section 1.7, Lingenfelter and Ramaty (1967), Ramaty and Lingenfelter (1973a, b), Hurford et al. (1973) were the first who have considered in detail positron production and annihilation during solar flares. It was found that the dominant source of small energy positrons with kinetic energy 0.2 MeV ≤ E ≤ 2 MeV in the periods of chromospheric flares is expected to be the β+ decay of nuclear interaction products such as 11C, 13N and 15O and high energy positrons of several tens MeV from π+ → μ+ → e+ decay, all of which are produced by interactions of accelerated protons, α-particles and heavy nuclei with the ambient solar atmosphere (Ramaty and Murphy 1987). The first process results from low energy interactions at ∼10 MeV, and the resultant positrons have typical energies of ∼1 MeV. On the other hand, the secondary ones are high energy proton interactions above 300 MeV and the positron energies are ∼30 MeV." @default.
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- W7524203 date "2010-01-01" @default.
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- W7524203 title "Positron Generation in the Nuclear Interactions of Flare Energetic Particles in the Solar Atmosphere" @default.
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