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      The power output of spine and fan magnetic reconnection solutions

      Craig, Ian J.D.; Fabling, R.B.; Watson, P.G.
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      power.pdf
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      DOI
       10.1086/304411
      Link
       www.journals.uchicago.edu
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      Craig, 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.
      Permanent Research Commons link: https://hdl.handle.net/10289/1380
      Abstract
      The 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.
      Date
      1997-08
      Type
      Journal Article
      Rights
      This article has been published in the Astrophysical Journal. Copyright 1997 The American Astronomical Society.
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      • Computing and Mathematical Sciences Papers [1454]
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