Turbulent reconnection. [Of solar corona]

Journal Article · Tue Mar 01 00:00:00 EST 1988 · Astrophys. J.; (United States)

DOI:https://doi.org/10.1086/166104· OSTI ID:7251711

Strauss, H R

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. 41 references.

• Research Organization: New York Univ., NY (USA)
• OSTI ID: 7251711
• Journal Information: Astrophys. J.; (United States), Vol. 326
• Country of Publication: United States
• Language: English

Related Subjects

71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
SOLAR CORONA
MAGNETIC RECONNECTION
MAGNETIC FIELDS
RESISTANCE HEATING
TEARING INSTABILITY
TURBULENCE
ATMOSPHERES
ELECTRIC HEATING
HEATING
INSTABILITY
PLASMA INSTABILITY
PLASMA MACROINSTABILITIES
STELLAR ATMOSPHERES
STELLAR CORONAE
640104* - Astrophysics & Cosmology- Solar Phenomena