Journal
ASTROPHYSICAL JOURNAL
Volume 801, Issue 2, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/801/2/145
Keywords
magnetic reconnection; magnetohydrodynamics (MHD); solar wind; Sun: corona
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Funding
- National Aeronautics and Space Administration
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This paper studies the growth rate of reconnection instabilities in thin current sheets in the presence of both resistivity and viscosity. In a previous paper, Pucci & Velli, it was argued that at sufficiently high Lundquist number S it is impossible to form current sheets with aspect ratios L/a that scale as L/a similar to S-alpha with alpha > 1/3 because the growth rate of the tearing mode would then diverge in the ideal limit S --> infinity. Here we extend their analysis to include the effects of viscosity, always present in numerical simulations along with resistivity, and which may play a role in the solar corona and other astrophysical environments. A finite Prandtl number allows current sheets to reach larger aspect ratios before becoming rapidly unstable in pileup-type regimes. Scalings with Lundquist and Prandtl numbers are discussed, as well as the transition to kinetic reconnection.
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