Mar 1988
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...326..412s&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 326, March 1, 1988, p. 412-417.
Other
81
Magnetic Field Reconnection, Solar Corona, Tearing Modes (Plasmas), Current Sheets, Plasma Turbulence, Resistance Heating
Scientific paper
The reconnection rate in the presence of tearing mode turbulence is calculated. Tearing modes can produce turbulence in three-dimensional sheared magnetic fields. They produce a turbulent anomalous electron viscosity or hyperresistivity. Using quasi-linear and direct interaction approximations, the scaling of the hyperresistivity with magnetic perturbation strength and other parameters is estimated. This yields a reconnection rate, or inflow Mach number M, scaling as delta B, the ratio of rms magnetic fluctuations to mean magnetic field. This can greatly exceed the Sweet-Parker rate. The rate of heating of the current sheet is also large and can be many orders of magnitude larger than in a Sweet-Parker current sheet. Hyperresistivity produced by tearing mode turbulence may explain both fast reconnection and the heating of the solar corona.
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