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The formation flare loops by magnetic reconnection and chromospheric ablationNoncoplanar compressible reconnection theory is combined here with simple scaling arguments for ablation and radiative cooling to predict average properties of hot and cool flare loops as a function of the coronal vector magnetic field. For a coronal field strength of 100 G, the temperature of the hot flare loops decreases from 1.2 x 10 to the 7th K to 4.0 x 10 to the 6th K as the component of the coronal magnetic field perpendicular to the plane of the loops increases from 0 percent to 86 percent of the total field. When the perpendicular component exceeds 86 percent of the total field or when the altitude of the reconnection site exceeds 10 to the 6th km, flare loops no longer occur. Shock-enhanced radiative cooling triggers the formation of cool H-alpha flare loops with predicted densities of roughly 10 to the 13th/cu cm, and a small gap of roughly 1000 km is predicted to exist between the footpoints of the cool flare loops and the inner edges of the flare ribbons.
Document ID
19890064449
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Forbes, T. G.
(Observatoire de Paris-Meudon France)
Malherbe, J. M.
(Paris Observatoire, Meudon, France)
Priest, E. R.
(Saint Andrews, University United Kingdom)
Date Acquired
August 14, 2013
Publication Date
January 1, 1989
Publication Information
Publication: Solar Physics
Volume: 120
Issue: 2 19
ISSN: 0038-0938
Subject Category
Solar Physics
Accession Number
89A51820
Funding Number(s)
CONTRACT_GRANT: NSF ATM-87-11089
CONTRACT_GRANT: NAGW-76
Distribution Limits
Public
Copyright
Other

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