Arbitrary-order Hilbert Spectral Analysis and Intermittency in Solar Wind Density Fluctuations

@article{Carbone2018ArbitraryorderHS,
  title={Arbitrary-order Hilbert Spectral Analysis and Intermittency in Solar Wind Density Fluctuations},
  author={Francesco Carbone and Luca Sorriso-Valvo and Tommaso Alberti and Fabio Lepreti and Christopher H. K. Chen and Zdeněk Něme{\vc}ek and Jana {\vS}afr{\'a}nkov{\'a}},
  journal={The Astrophysical Journal},
  year={2018},
  volume={859}
}
The properties of inertial- and kinetic-range solar wind turbulence have been investigated with the arbitrary-order Hilbert spectral analysis method, applied to high-resolution density measurements. Due to the small sample size and to the presence of strong nonstationary behavior and large-scale structures, the classical analysis in terms of structure functions may prove to be unsuccessful in detecting the power-law behavior in the inertial range, and may underestimate the scaling exponents… 

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References

SHOWING 1-10 OF 50 REFERENCES

Intermittency, non-Gaussian statistics and fractal scaling of MHD fluctuations in the solar wind

Abstract. This paper gives a review of some recent work on intermittency, non-Gaussian statistics, and fractal scaling of solar wind magnetohydrodynamic turbulence. Model calculations and theories

Intermittency in the solar wind turbulence through probability distribution functions of fluctuations

Intermittency in fluid turbulence can be emphasized through the analysis of Probability Distribution Functions (PDF) for velocity fluctuations, which display a strong non‐gaussian behavior at small

Small-Scale Energy Cascade of the Solar Wind Turbulence

Magnetic fluctuations in the solar wind are distributed according to Kolmogorov’s power law f−5/3 below the ion cyclotron frequency fci. Above this frequency, the observed steeper power law is

Second-order structure function in fully developed turbulence.

An analysis of passive scalar (temperature) turbulence time series is presented to show the influence of large-scale structures in real turbulence and the efficiency of the Hilbert-based methodology, and corresponding scaling exponents ζ(θ)(q) provided by the Hilbert -based approach indicate that the Passive scalar turbulence field may be less intermittent than what was previously believed.

RADIAL EVOLUTION OF THE INTERMITTENCY OF DENSITY FLUCTUATIONS IN THE FAST SOLAR WIND

We study the radial evolution of the intermittency of density fluctuations in the fast solar wind. The study is performed by analyzing the plasma density measurements provided by Helios 2 in the

An amplitude-frequency study of turbulent scaling intermittency using Empirical Mode Decomposition and Hilbert Spectral Analysis

Hilbert-Huang transform is a method that has been introduced recently to decompose nonlinear, nonstationary time series into a sum of different modes, each one having a characteristic frequency. Here

Solar Wind Turbulence and the Role of Ion Instabilities

Solar wind is probably the best laboratory to study turbulence in astrophysical plasmas. In addition to the presence of magnetic field, the differences with neutral fluid isotropic turbulence are:

SOLAR WIND DENSITY SPECTRA AROUND THE ION SPECTRAL BREAK

This paper presents a large statistical analysis of ≈ 5800 ?> frequency spectra of the solar wind density fluctuations in the range 0.001–5 Hz (corresponding to spatial scales of 100–5 × 105 km). The

Intermittency, scaling, and the Fokker-Planck approach to fluctuations of the solar wind bulk plasma parameters as seen by the WIND spacecraft.

A model independent method of differencing and rescaling is applied to identify self-similarity in the probability density functions (PDF) of fluctuations in solar wind bulk plasma parameters as seen by the WIND spacecraft.