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dc.contributor.authorCraig, Ian J.D.
dc.contributor.authorFabling, R.B.
dc.contributor.authorWatson, P.G.
dc.date.accessioned2008-11-18T03:30:34Z
dc.date.available2008-11-18T03:30:34Z
dc.date.issued1997-08
dc.identifier.citationCraig, I. J. D., Fabling, R. B. & Watson, P. G.(1997). The power output of spine and fan magnetic reconnection solutions. The Astrophysical Journal, 485(1), 383- 388.en_US
dc.identifier.urihttps://hdl.handle.net/10289/1380
dc.description.abstractThe ability of three-dimensional magnetic “spine” and “fan” reconnection solutions to provide flarelike energy release is discussed. It is pointed out, on the basis of exact analytic solutions, that fast dissipation is possible only if the hydromagnetic pressure in the reconnection region becomes unbounded in the limit of small plasma resistivities. The implication is that some “saturation” of the power output is inevitable for realistic coronal plasmas. Estimates of the saturated power, based on limiting the flux pileup in the field, suggest that the geometry of the spine reconnection mechanism precludes significant flare energy release. However, the current sheet structures involved in fan reconnection seem able to release sufficient magnetic energy fast enough to account for modest flares, even under the conservative assumption of classical plasma resistivities.en_US
dc.format.mimetypeapplication/pdf
dc.language.isoen
dc.relation.urihttp://www.journals.uchicago.edu/doi/abs/10.1086/304411en_US
dc.rightsThis article has been published in the Astrophysical Journal. Copyright 1997 The American Astronomical Society.en_US
dc.subjectMHD—plasmasen_US
dc.titleThe power output of spine and fan magnetic reconnection solutionsen_US
dc.typeJournal Articleen_US
dc.identifier.doi10.1086/304411en_US
dc.relation.isPartOfAstrophysical Journalen_NZ
pubs.begin-page383en_NZ
pubs.elements-id39940
pubs.end-page388en_NZ
pubs.issue1en_NZ
pubs.volume485en_NZ


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