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Area of Science:

  • Space Physics
  • Plasma Physics
  • Astrophysics

Background:

  • Spacecraft observations reveal magnetic reconnection events in the solar wind with extended "X lines" and wide outflows.
  • These phenomena occur at scales significantly larger than ion scales, suggesting the influence of turbulence.

Purpose of the Study:

  • To investigate the role of turbulence in magnetic reconnection at large scales.
  • To understand the detailed mechanisms driving the broadening of reconnection regions and X lines.

Main Methods:

  • A case study of an inertial-range magnetic reconnection event was performed using a magnetohydrodynamic (MHD) simulation.
  • Analysis focused on the behavior of field lines, magnetic flux freezing, and the structure of the reconnection zone.

Main Results:

  • Stochastic wandering of magnetic field lines was observed.
  • The standard magnetic flux freezing condition was found to break down due to Richardson dispersion.
  • A broadened reconnection zone containing multiple current sheets was identified.

Conclusions:

  • The simulation results show that turbulence leads to a breakdown of magnetic flux freezing and a broadened reconnection region.
  • The coarse-grained magnetic geometry resembles large-scale solar wind reconnection, characterized by a hyperbolic flux tube or apparent X line extending over integral length scales.