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Deexcitation gamma-ray line emission from solar flare magnetic loopsA Monte Carlo simulation that follows individual ions throughout a solar flare magnetic loop is developed. Included are energy losses due to Coulomb collisions, removal by nuclear reactions, magnetic mirroring in the convergent flux tubes, and MHD pitch-angle scattering in the corona. Calculations are made of the depth distribution of nuclear deexcitation line production, the time dependence of the production of the lines, and the escape probability of the line photons from the solar atmosphere. It is found that the inclusion of mirroring and pitch-angle scattering leads to time profiles which are in good agreement with observations. This suggests that the decaying portions of the time profiles of gamma-ray emission observed from solar flares could be governed by transport and not by acceleration.
Document ID
19890054026
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Hua, X.-M.
(Maryland, University College Park, United States)
Ramaty, R.
(NASA Goddard Space Flight Center Greenbelt, MD, United States)
Lingenfelter, R. E.
(California, University San Diego, United States)
Date Acquired
August 14, 2013
Publication Date
June 1, 1989
Publication Information
Publication: Astrophysical Journal, Part 1
Volume: 341
ISSN: 0004-637X
Subject Category
Solar Physics
Accession Number
89A41397
Funding Number(s)
CONTRACT_GRANT: NAG5-945
CONTRACT_GRANT: NGR-21-002-316
CONTRACT_GRANT: NSF ATM-87-17676
Distribution Limits
Public
Copyright
Other

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