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Reconnection-Driven Magnetohydrodynamic Turbulence in a Simulated Coronal-Hole Jet.

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  • 1Catholic University of America, 620 Michigan Avenue NE, Washington, DC 20064 USA.

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Coronal hole jets generate magnetic turbulence, driving microstreams and waves in solar wind. This study confirms reconnection-driven turbulence and its properties, matching observations from the Ulysses spacecraft.

Keywords:
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Area of Science:

  • Solar physics
  • Plasma astrophysics
  • Heliophysics

Background:

  • Extreme-ultraviolet and X-ray jets are common in the Sun's coronal holes.
  • These jets may cause microstreams and torsional Alfvén waves in the solar wind.

Purpose of the Study:

  • To statistically analyze a simulated coronal hole jet.
  • To understand the signatures and properties of these jets for prediction.

Main Methods:

  • Detailed statistical analysis of a simulated jet using an adaptively refined magnetohydrodynamics model.
  • Calculation of spatial correlations of magnetic fluctuations.

Main Results:

  • Confirmed generation and persistence of 3D, reconnection-driven magnetic turbulence.
  • Magnetic fluctuation correlations align with the Müller-Biskamp scaling model.
  • Anisotropy and current sheet orientation match nonlinear Alfvén waves and the jet's collimated structure.

Conclusions:

  • The simulated jet's turbulence properties are consistent with observations.
  • Turbulence in the jet wake quantitatively matches fast solar wind turbulence observed by Ulysses.