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      Viscous dissipation in 3D spine reconnection solutions

      Craig, Ian J.D.; Lopez, N.
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      Astronomy-Astrophysics-560.pdf
      Published version, 1.457Mb
      DOI
       10.1051/0004-6361/201321815
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      Craig, I. J. D., & Lopez, N. (2013). Viscous dissipation in 3D spine reconnection solutions. ASTRONOMY & ASTROPHYSICS, 560. http://doi.org/10.1051/0004-6361/201321815
      Permanent Research Commons link: https://hdl.handle.net/10289/9359
      Abstract
      Aims. We consider the influence of viscous dissipation on “spine” reconnection solutions in coronal plasmas. It is known from 2D and 3D “fan” reconnection studies that viscous losses can be important. We extend these arguments to 3D “spine” reconnection solutions. Methods. Steady 3D spine reconnection models were constructed by time relaxation of the governing visco-resistive MHD equations. Scaling laws were derived that compare the relative importance of viscous and resistive damping. Results. It is shown that viscous dissipation in spine reconnection models can dominate resistive damping by many orders of magnitude. A similar conclusion, but with less severe implications, applies to current sheet “fan” solutions. These findings are not sensitive to whether classical or Braginskii viscosity is employed.
      Date
      2013-12-01
      Type
      Journal Article
      Publisher
      European Southern Observatory
      Rights
      Reproduced with permission from Astronomy & Astrophysics, © ESO 2013
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      • Computing and Mathematical Sciences Papers [1455]
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