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An interacting loop model for solar flare burstsA schematic model is presented which attempts to explain the quasi-periodic behavior (on a timescale of less than or approximately equal to 10 s) frequency observed in solar hard X-ray bursts. It is shown how, as a result of the strong heating produced during a solar flare burst, the local gas pressure can transiently attain very large values in regions corresponding to the upper preflare chromosphere. The effectiveness of the surrounding magnetic field at confining this high pressure plasma is therefore reduced and the flaring loop becomes free to expand laterally. In so doing it may drive magnetic field lines into neighboring, non-flaring, loops in the same active region, causing magnetic reconnection to take place and triggering another flare burst. The features of this interacting loop model are found to be in good agreement with the energetics and time structure of flare-associated solar hard X-ray bursts.
Document ID
19820033636
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
Authors
Emslie, A. G.
(Stanford University Stanford, CA, United States)
Date Acquired
August 10, 2013
Publication Date
January 1, 1981
Publication Information
Publication: Astrophysical Letters
Volume: 22
Issue: 2, 19
Subject Category
Solar Physics
Accession Number
82A17171
Funding Number(s)
CONTRACT_GRANT: NAGW-92
CONTRACT_GRANT: N00014-75-C-0673
CONTRACT_GRANT: NGL-05-020-272
Distribution Limits
Public
Copyright
Other

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