Shapes of 20Ne de-excitation line in solar flare

Shapes of 20Ne de-excitation line in solar flare Since almost all de-excitation lines from nuclear states excited by flare-accelerated protons and α $\alpha $ -particles are emitted promptly after nuclear collisions, the emission photon’s energy depends on the velocity of the recoiling nucleus. The energies and widths of γ $\gamma $ -ray lines provide a wealth of information on the directionality and spectra of ions in solar flares. In this paper, we use TALYS code to improve the cross sections of γ $\gamma $ -ray lines production, and calculate the shapes of the 1.634 MeV line from de-excitation of 20Ne as a function of ion’s energy spectra and the heliocentric angle. Taking this line shape as an example, we try to develop a new method of line shape analysis to study the properties of accelerated ions in solar flares. Astrophysics and Space Science Springer Journals

Shapes of 20Ne de-excitation line in solar flare

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Springer Netherlands
Copyright © 2017 by Springer Science+Business Media B.V.
Physics; Astrophysics and Astroparticles; Astronomy, Observations and Techniques; Cosmology; Space Sciences (including Extraterrestrial Physics, Space Exploration and Astronautics) ; Astrobiology
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