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On the acceleration of thermal coronal ions by flare induced shock wavesThe energy spectra of solar flare ions are calculated by assuming that the process which accelerates solar wind ions to MeV/ nucleon energies in the interplanetary corotating interaction region (CIR) also occurs in flare induced magnetosonic fast-mode (MFM) shocks in the corona. Solar wind ions are considered to be accelerated to MeV/nucleon energies by wave-particle interactions in the shock front and the downstream flow, being compressed between upstream and downstream magnetic field irregularities, and then accelerated by the shock drift acceleration mechanism. The energy spectra of the accelerated ions is calculated from the number of shock encounters as a function of the post- and preacceleration energies. A best fit by an exponential in momentum is determined for ions in the 50 MeV to a few GeV range, and from 20-80 MeV by a suitable power law in kinetic energy with a mean spectral index. Comparisons with observed solar protons show good agreement.
Document ID
19820039122
Acquisition Source
Legacy CDMS
Document Type
Conference Proceedings
Authors
Decker, R. B.
(Johns Hopkins University Applied Physics Laboratory, Laurel, MD, United States)
Pesses, M. E.
(Maryland, University College Park, MD, United States)
Armstrong, T. P.
(Kansas, University Lawrence, KS, United States)
Date Acquired
August 10, 2013
Publication Date
January 1, 1981
Subject Category
Solar Physics
Meeting Information
Meeting: International Cosmic Ray Conference
Location: Paris
Country: France
Start Date: July 13, 1981
End Date: July 25, 1981
Accession Number
82A22657
Funding Number(s)
CONTRACT_GRANT: NAS5-20062
CONTRACT_GRANT: NSF ATM-79-25987
Distribution Limits
Public
Copyright
Other

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