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Magnetic reconnection in the two-dimensional Kelvin-Helmholtz instability
1Theoretical Division, Los Alamos National Laboratory, Los Alamos, New Mexico 87545, USA.
Physical Review Letters
|June 13, 2002
Summary
Magnetic reconnection in Kelvin-Helmholtz instability shows peak rates depend on flow shear, not resistivity. This finding differs significantly between low and high magnetic Reynolds numbers (S).
Area of Science:
- Plasma Physics
- Astrophysics
- Fluid Dynamics
Background:
- The Kelvin-Helmholtz instability is a fundamental process in astrophysical and laboratory plasmas.
- Magnetic reconnection, a key energy release mechanism, is often studied in conjunction with plasma instabilities.
- Previous studies noted transient magnetic reconnection during Kelvin-Helmholtz instability on the instability's timescale.
Purpose of the Study:
- To investigate the peak magnetic reconnection rate during the two-dimensional Kelvin-Helmholtz instability.
- To determine the dependence of this peak reconnection rate on plasma resistivity and initial flow shear.
- To explore the impact of varying magnetic Reynolds numbers (S) on the instability's evolution.
Main Methods:
- Simulations using reduced Magnetohydrodynamic (MHD) equations with constant resistivity and viscosity.
- Analysis of super-Alfvénic flow conditions.
- Examination of reconnection rates relative to initial vortex formation and flow shear.
Main Results:
- The peak magnetic reconnection rate is independent of resistivity for the range studied.
- The peak reconnection rate is primarily a function of the initial flow shear.
- A fundamental difference in evolutionary behavior is observed between low (S=200) and high (S=10,000) magnetic Reynolds numbers.
Conclusions:
- Peak reconnection rates in Kelvin-Helmholtz instability are governed by flow shear, not resistivity.
- The magnetic Reynolds number significantly influences the overall dynamics of the instability and reconnection process.
- These findings have implications for understanding energy dissipation in various plasma environments.
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