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Characteristics of gamma-ray line flaresObservations of solar gamma rays by the Solar Maximum Mission (SMM) demonstrate that energetic protons and ions are rapidly accelerated during the impulsive phase. To understand the acceleration mechanisms for these particles, the characteristics of the gamma ray line flares observed by SMM were studied. Some very intense hard X-ray flares without detectable gamma ray lines were also investigated. Gamma ray line flares are distinguished from other flares by: (1) intense hard X-ray and microwave emissions; (2) delay of high energy hard X-rays; (3) emission of type 2 and/or type 4 radio bursts; and (4) flat hard X-ray spectra (average power law index: 3.1). The majority of the gamma ray line flares shared all these characteristics, and the remainder shared at least three of them. Positive correlations were found between durations of spike bursts and spatial sizes of flare loops as well as between delay times and durations of spike bursts.
Document ID
19840006030
Acquisition Source
Legacy CDMS
Document Type
Contractor Report (CR)
Authors
Bai, T. (Stanford Univ. Greenbelt, MD, United States)
Dennis, B. (NASA Goddard Space Flight Center)
Date Acquired
September 4, 2013
Publication Date
October 1, 1983
Subject Category
Solar Physics
Report/Patent Number
SU-SUIPR-961
AD-A136266
NASA-CR-174608
NAS 1.26:174608
Accession Number
84N14098
Funding Number(s)
CONTRACT_GRANT: N00014-75-C-0673
CONTRACT_GRANT: NGL-05-020-272
CONTRACT_GRANT: NAGW-92
Distribution Limits
Public
Copyright
Work of the US Gov. Public Use Permitted.

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