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Spectral evolution of energetic protons in solar flares
Gan, WQ
AbstractThe energy spectrum of accelerated protons in solar flares assuming it is either a Bessel function or a power law, is usually deduced from the fluence ratio of the 2.223 MeV neutron capture line, which is of a delayed nature, to 4-7 MeV nuclear emissions. The spectral index obtained in this way is an integration over time. So far almost no detailed information on how the energetic particle spectrum changes with time is available. In this paper we develop a method to study this question and apply it to observations of Gamma-Ray Spectrometer/Solar Maximum Mission flares. For three intense gamma-ray line flares, with a temporal resolution of 16.384 s, we find for the first time that from the maximum (even from the rising phase) to the decay phase, the energy spectra of accelerated protons evolve from soft to hard. This gradual hardening with time, in contrast to the general soft-hard-soft variation of the spectra of energetic electrons, represents a new constraint for the acceleration mechanism in solar flares.
KeywordAcceleration Of Particles Sun, Flares Sun, Particle Emission Sun, X-Rays, Gamma Rays
Subject AreaAstronomy & Astrophysics
WOS HeadingsScience & Technology ; Physical Sciences
Indexed BySCI
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS IDWOS:000073048100036
Citation statistics
Cited Times:21[WOS]   [WOS Record]     [Related Records in WOS]
Document Type期刊论文
AffiliationAcad Sinica, Purple Mt Observ, Nanjing 210008, Peoples R China
Recommended Citation
GB/T 7714
Gan, WQ. Spectral evolution of energetic protons in solar flares[J]. ASTROPHYSICAL JOURNAL,1998,496(2):992-997.
APA Gan, WQ.(1998).Spectral evolution of energetic protons in solar flares.ASTROPHYSICAL JOURNAL,496(2),992-997.
MLA Gan, WQ."Spectral evolution of energetic protons in solar flares".ASTROPHYSICAL JOURNAL 496.2(1998):992-997.
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