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Updated: Feb 14, 2026
13:02
Three-dimensional Particle Tracking Velocimetry for Turbulence Applications: Case of a Jet Flow
Published on: February 27, 2016
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Reconnection-Driven Magnetohydrodynamic Turbulence in a Simulated Coronal-Hole Jet
Vadim M Uritsky1,2, Merrill A Roberts1,2, C Richard DeVore2
1Catholic University of America, 620 Michigan Avenue NE, Washington, DC 20064 USA.
The Astrophysical Journal
|February 13, 2018
Summary
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.
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.
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