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Updated: Apr 15, 2026
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Non-equilibrium Microwave Plasma for Efficient High Temperature Chemistry
Published on: August 1, 2017
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Anisotropy in solar wind plasma turbulence
S Oughton1, W H Matthaeus2, M Wan2
1Department of Mathematics, University of Waikato, Hamilton 3240, New Zealand seano@waikato.ac.nz.
Summary
This review examines solar wind fluctuations, finding energy concentrated in transverse components in the inertial range. Dissipation range observations show decreasing anisotropy near the electron gyroradius, with mixed results for spectral anisotropy.
Area of Science:
- Plasma Physics
- Space Physics
- Astrophysics
Background:
- Solar wind exhibits complex fluctuations across different scales.
- Understanding anisotropy is crucial for solar wind models.
Purpose of the Study:
- To review spectral and variance anisotropy in solar wind fluctuations.
- To discuss interpretations of observed phenomena in the inertial and dissipation ranges.
- To present new simulation results on variance anisotropy evolution.
Main Methods:
- Review of existing theory, simulations, and observational data.
- Analysis of solar wind fluctuations in the inertial and dissipation ranges.
- Presentation of new simulation results with varying initial conditions.
Main Results:
- Inertial range: Fluctuation energy is predominantly in quasi-perpendicular modes and transverse components.
- Inertial range: Parallel energy transfer and levels are weak.
- Dissipation range: Variance anisotropy decreases towards isotropy near the electron gyroradius; spectral anisotropy results are mixed.
Conclusions:
- The study synthesizes current understanding of solar wind anisotropy.
- It highlights agreement in the inertial range and mixed findings in the dissipation range.
- New simulations provide insights into variance anisotropy evolution under different solar wind conditions.
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