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The starting conditions for an optically small solar gamma ray flareIt is suggested that optically small gamma-ray flares result from gradual pre-flare acceleration of protons over approximately 1,000 s by a series of magnetohydrodynamic shocks in the low corona. A fraction of the accelerated protons are trapped in the corona where they form a seed population for future acceleration. If the shock acceleration is sufficiently rapid proton energies may exceed the gamma-ray production threshold and trigger gamma-ray emission. This occurs without the total flare energy being necessarily large. Magnetic field geometry is an important parameter.
Document ID
19850026438
Acquisition Source
Legacy CDMS
Document Type
Conference Paper
Authors
Simnett, G. M. (Birmingham Univ.)
Ryan, J. M. (New Hampshire Univ.)
Date Acquired
August 12, 2013
Publication Date
August 1, 1985
Publication Information
Publication: 19th Intern. Cosmic Ray Conf - Vol. 4
Subject Category
Solar Physics
Report/Patent Number
SH-1.3-2
Accession Number
85N34751
Distribution Limits
Public
Copyright
Work of the US Gov. Public Use Permitted.

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IDRelationTitle19850026416Collected WorksNinteenth International Cosmic Ray Conference. SH Sessions, Volume 4
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