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Solar Wind Turbulence and Complexity Probed with Rank-Ordered Multifractal Analysis (ROMA).

Marius Echim1,2, Costel Munteanu2, Gabriel Voitcu2

  • 1Royal Belgian Institute for Space Aeronomy, Avenue Circulaire 3, 1180 Bruxelles, Belgium.

Entropy (Basel, Switzerland)
|November 27, 2024
PubMed
Summary
This summary is machine-generated.

Rank-Ordered Multifractal Analysis (ROMA) reveals distinct solar wind turbulence patterns. Fast solar wind shows scale-dependent fluctuations, while slow solar wind exhibits fully developed multifractal turbulence.

Keywords:
complexityintermittencymultifractal analysisrank-ordered multifractal analysissolar windturbulence

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Area of Science:

  • Space Physics
  • Plasma Physics
  • Astrophysics

Background:

  • Solar wind turbulence is a complex phenomenon crucial for understanding energy transfer in space.
  • Characterizing multifractality and scale-invariance in turbulent plasmas is essential for astrophysical studies.

Purpose of the Study:

  • To apply Rank-Ordered Multifractal Analysis (ROMA) to characterize solar wind turbulence.
  • To compare the multifractal properties of fast and slow solar wind using spacecraft data.

Main Methods:

  • Rank-Ordered Multifractal Analysis (ROMA) was employed to analyze fluctuations.
  • Range-limited structure-function analysis was used to determine mono-fractal indices.
  • Data from Ulysses (fast solar wind) and Venus Express (slow solar wind) spacecraft were analyzed.

Main Results:

  • Fast solar wind exhibits scale-dependent fluctuations: persistent at kinetic scales and anti-persistent at inertial scales.
  • Slow solar wind shows fully developed multifractal turbulence with a transition in Hurst index.
  • Small-scale fluctuations in slow solar wind tend towards mono-fractal behavior.

Conclusions:

  • ROMA effectively differentiates multifractal characteristics of fast and slow solar wind turbulence.
  • The findings provide insights into the scale-dependent nature and complexity of solar wind dynamics.
  • Differentiation of turbulence structures has implications for understanding plasma behavior in heliospheric environments.