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Finite size scaling in the solar wind magnetic field energy\ud density as seen by WIND

By B. Hnat, Sandra C. Chapman, G. (George) Rowlands, Nicholas W. Watkins and W. M. (William M.) Farrell

Abstract

Statistical properties of the interplanetary magnetic field fluctuations can provide an important insight into the solar wind turbulent cascade. Recently, analysis of the Probability Density Functions (PDF) of the velocity and magnetic field fluctuations has shown that these exhibit non-Gaussian properties on small time scales while large scale features appear to be uncorrelated. Here we apply the finite size scaling technique to explore the scaling of the magnetic field energy density fluctuations as seen by WIND. We find a single scaling sufficient to collapse the curves over the entire investigated range. The rescaled PDF follow a non Gaussian distribution with asymptotic behavior well described by the Gamma distribution arising from a finite range Lévy walk. Such mono scaling suggests that a Fokker-Planck approach can be applied to study the PDF dynamics. These results strongly suggest the existence of a common, nonlinear process on the time scale up to 26 hours

Topics: QB
Publisher: American Geophysical Union
Year: 2002
OAI identifier: oai:wrap.warwick.ac.uk:3866

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Citations

  1. (1962). A refinement of previous hypotheses concerning the local structure of turbulence in a viscous incompressible fluid at high Reynolds number, doi
  2. (2000). An Introduction to Econophysics, doi
  3. (1998). Conditional statistics of velocity fluctuations in turbulence, doi
  4. (2000). Critical Phenomena in Natural Sciences; Chaos, Fractals, Selforganization and Disorder: Concepts and Tools, doi
  5. (2001). Distribution of magnetic field components in the solar wind plasma, doi
  6. (1998). Dynamical Systems Approach to Turbulence, doi
  7. Evidence for a solar wind origin of the power law burst lifetime distribution of the AE indices, doi
  8. (2001). Fractional Fokker-Planck equation for nonlinear stochastic differential equations driven by non-Gaussian Le ´vy stable noise, doi
  9. (1998). Fracton excitations as a driving mechanism for the self-organized dynamical structuring in the solar wind, doi
  10. (2001). Intermittency in plasma turbulence, doi
  11. (1999). Intermittency in the solar wind turbulence through probability distribution functions of fluctuations, doi
  12. (2002). Le ´vy Statistics and Laser Cooling, doi
  13. (2001). Lognormal and multifractal distributions of the heliospheric magnetic field, doi
  14. (1999). Magnetohydrodynamic Turbulence in the solar wind, doi
  15. Power law distribution of burst duration and interburst interval in the solar wind: Turbulence or dissipative self-organized criticality?, doi
  16. (1995). Scaling behaviour in the dynamics of an economic index, doi
  17. (1972). Statistical Self-Similarity and Inertial Subrange Turbulence, doi
  18. (1995). The legacy of A.N. Kolmogorov, doi
  19. (1995). The WIND Magnetic Field Investigation, Space Sci. doi
  20. (1990). Velocity Probability Density Functions of High Reynolds Number Turbulence, doi
  21. (1995). Waves and Turbulence in the Solar Wind: Observations and Theories, doi

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