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Title:
Turbulent reconnection
Authors:
Strauss, H. R.
Affiliation:
AA(New York University, NY)
Publication:
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 326, March 1, 1988, p. 412-417. (ApJ Homepage)
Publication Date:
03/1988
Category:
Solar Physics
Origin:
STI
NASA/STI Keywords:
Magnetic Field Reconnection, Solar Corona, Tearing Modes (Plasmas), Current Sheets, Plasma Turbulence, Resistance Heating
DOI:
10.1086/166104
Bibliographic Code:
1988ApJ...326..412S

Abstract

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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