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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 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 Zum Text:
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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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titleShapes of 20 Ne de-excitation line in solar flare
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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pages1-6
date2017-09