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Shapes of 20 Ne 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 pro... Full description

Journal Title: Astrophysics and Space Science 2017, Vol.362(9), pp.1-6
Main Author: Chen, Wei
Other Authors: Gan, Wei
Format: Electronic Article Electronic Article
Language: English
Subjects:
ID: ISSN: 0004-640X ; E-ISSN: 1572-946X ; DOI: 10.1007/s10509-017-3126-8
Link: http://dx.doi.org/10.1007/s10509-017-3126-8
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recordid: springer_jour10.1007/s10509-017-3126-8
title: Shapes of 20 Ne de-excitation line in solar flare
format: Article
creator:
  • Chen, Wei
  • Gan, Wei
subjects:
  • Gamma-rays
  • Solar flare
  • Line shape
ispartof: Astrophysics and Space Science, 2017, Vol.362(9), pp.1-6
description: 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 20 Ne 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.
language: eng
source:
identifier: ISSN: 0004-640X ; E-ISSN: 1572-946X ; DOI: 10.1007/s10509-017-3126-8
fulltext: fulltext
issn:
  • 1572-946X
  • 1572946X
  • 0004-640X
  • 0004640X
url: Link


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subjectGamma-rays ; Solar flare ; Line shape
descriptionSince 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 20 Ne 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.
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abstractSince 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 20 Ne 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.
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doi10.1007/s10509-017-3126-8
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date2017-09