scholarly journals Statistical Analysis of the Magnetic and Velocity Field Fluctuations for the Solar Wind Turbulence

2012 ◽  
Vol 4 (3) ◽  
Author(s):  
Mahdi Momeni
Keyword(s):  
Solar Wind ◽  
Statistical Analysis ◽  
Velocity Field ◽  
Solar Wind Turbulence ◽  
Wind Turbulence ◽  
Field Fluctuations

scholarly journals Scale dependent anisotropy of electric field fluctuations in solar wind turbulence

2021 ◽  
Author(s):  
Deepali Deepali ◽  
Supratik Banerjee
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Electric Field ◽  
Electric Power ◽  
Flow Direction ◽  
Power Spectra ◽  
Solar Wind Turbulence ◽  
Wind Turbulence ◽  
Field Fluctuations ◽  
Spacecraft Data

<p>We study the variation of average powers and spectral indices of electric field fluctuations with respect to the angle between average flow direction and the mean magnetic field in solar wind turbulence. Cluster spacecraft data from the years 2002 and 2007 are used for the present analysis. We perform a scale dependent study with respect to the local mean magnetic field using wavelet analysis technique. Prominent anisotropies are found for both the spectral index and power levels of the electric power spectra. Similar to the magnetic field fluctuations, the parallel (or antiparallel) electric fluctuation spectrum is found to be steeper than the perpendicular spectrum. However the parallel (or antiparallel) electric power is found to be greater than the perpendicular one. Below 0.1 Hz, the slope of the parallel electric power spectra deviates substantially from that of the total magnetic power spectra, supporting the existence of Alfvénic turbulence.</p>

Statistical Analysis of the High‐Frequency Spectral Break of the Solar Wind Turbulence at 1 AU

2008 ◽  
Vol 675 (2) ◽  
pp. 1576-1583 ◽  
Author(s):  
S. A. Markovskii ◽  
Bernard J. Vasquez ◽  
Charles W. Smith
Keyword(s):  
Solar Wind ◽  
Statistical Analysis ◽  
High Frequency ◽  
Solar Wind Turbulence ◽  
Spectral Break ◽  
Wind Turbulence

scholarly journals Statistical analysis of transfer of fluctuations in solar wind turbulence

2008 ◽  
Vol 15 (4) ◽  
pp. 607-613 ◽  
Author(s):  
M. Strumik ◽  
W. M. Macek
Keyword(s):  
Experimental Data ◽  
Solar Wind ◽  
Statistical Analysis ◽  
Markov Processes ◽  
Kolmogorov Equation ◽  
Slow Solar Wind ◽  
Local Character ◽  
Solar Wind Turbulence ◽  
Wind Turbulence ◽  
Turbulent Cascade

Abstract. We present results of statistical analysis of the transfer of fluctuations in solar wind turbulence. We investigate the dynamics of the slow solar wind using an approach based on the Markov processes theory and experimental data measured by ACE spacecraft. In particular, we test whether the Chapman-Kolmogorov equation is approximately satisfied for the turbulent cascade. We consider the following cases of transfer of fluctuations: magnetic-to-magnetic, velocity-to-velocity, velocity-to-magnetic, and magnetic-to-velocity. In all these cases, the obtained results confirm local character of the transfer of fluctuations.

scholarly journals Generation and evolution of anisotropic turbulence and related energy transfer in drifting proton-alpha plasmas

2018 ◽  
Vol 613 ◽  
pp. A10 ◽  
Author(s):  
Y. G. Maneva ◽  
S. Poedts
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Plasma Heating ◽  
Plasma Temperature ◽  
Plasma Properties ◽  
Anisotropic Turbulence ◽  
Solar Wind Turbulence ◽  
Background Magnetic Field ◽  
Wind Turbulence ◽  
Field Fluctuations

The power spectra of magnetic field fluctuations in the solar wind typically follow a power-law dependence with respect to the observed frequencies and wave-numbers. The background magnetic field often influences the plasma properties, setting a preferential direction for plasma heating and acceleration. At the same time the evolution of the solar-wind turbulence at the ion and electron scales is influenced by the plasma properties through local micro-instabilities and wave-particle interactions. The solar-wind-plasma temperature and the solar-wind turbulence at sub- and sup-ion scales simultaneously show anisotropic features, with different components and fluctuation power in parallel with and perpendicular to the orientation of the background magnetic field. The ratio between the power of the magnetic field fluctuations in parallel and perpendicular direction at the ion scales may vary with the heliospheric distance and depends on various parameters, including the local wave properties and nonthermal plasma features, such as temperature anisotropies and relative drift speeds. In this work we have performed two-and-a-half-dimensional hybrid simulations to study the generation and evolution of anisotropic turbulence in a drifting multi-ion species plasma. We investigate the evolution of the turbulent spectral slopes along and across the background magnetic field for the cases of initially isotropic and anisotropic turbulence. Finally, we show the effect of the various turbulent spectra for the local ion heating in the solar wind.

scholarly journals Scale-dependent angle of alignment between velocity and magnetic field fluctuations in solar wind turbulence

2009 ◽  
Vol 114 (A1) ◽  
pp. n/a-n/a ◽  
Author(s):  
J. J. Podesta ◽  
B. D. G. Chandran ◽  
A. Bhattacharjee ◽  
D. A. Roberts ◽  
M. L. Goldstein
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Solar Wind Turbulence ◽  
Wind Turbulence ◽  
Field Fluctuations

scholarly journals Three-Dimensional Anisotropy and Scaling Properties of Solar Wind Turbulence at Kinetic Scales in the Inner Heliosphere: Parker Solar Probe Observations

2022 ◽  
Vol 924 (2) ◽  
pp. L21
Author(s):  
J. Zhang ◽  
S. Y. Huang ◽  
J. S. He ◽  
T. Y. Wang ◽  
Z. G. Yuan ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Three Dimensional ◽  
Order Structure ◽  
Parallel Magnetic Field ◽  
Transition Range ◽  
Solar Wind Turbulence ◽  
Wind Turbulence ◽  
Field Fluctuations ◽  
Inner Heliosphere

Abstract We utilize the data from the Parker Solar Probe mission at its first perihelion to investigate the three-dimensional (3D) anisotropies and scalings of solar wind turbulence for the total, perpendicular, and parallel magnetic-field fluctuations at kinetic scales in the inner heliosphere. By calculating the five-point second-order structure functions, we find that the three characteristic lengths of turbulence eddies for the total and the perpendicular magnetic-field fluctuations in the local reference frame ( L ˆ ⊥ , l ˆ ⊥ , l ˆ ∣ ∣ ) defined with respect to the local mean magnetic field B local feature as l ∣∣ > L ⊥ > l ⊥ in both the transition range and the ion-to-electron scales, but l ∣∣ > L ⊥ ≈ l ⊥ for the parallel magnetic-field fluctuations. For the total magnetic-field fluctuations, the wave-vector anisotropy scalings are characterized by l ∣ ∣ ∝ l ⊥ 0.78 and L ⊥ ∝ l ⊥ 1.02 in the transition range, and they feature as l ∣ ∣ ∝ l ⊥ 0.44 and L ⊥ ∝ l ⊥ 0.73 in the ion-to-electron scales. Still, we need more complete kinetic-scale turbulence models to explain all these observational results.

Observational Test for a Random Sweeping Model in Solar Wind Turbulence

2016 ◽  
Vol 116 (12) ◽  
Author(s):  
C. Perschke ◽  
Y. Narita ◽  
U. Motschmann ◽  
K. H. Glassmeier
Keyword(s):  
Solar Wind ◽  
Observational Test ◽  
Solar Wind Turbulence ◽  
Wind Turbulence

Erratum: “3D Anisotropy of Solar Wind Turbulence, Tubes, or Ribbons?” (2018, ApJ, 853, 85)

2018 ◽  
Vol 867 (2) ◽  
pp. 168 ◽  
Author(s):  
Andrea Verdini ◽  
Roland Grappin ◽  
Olga Alexandrova ◽  
Sonny Lion
Keyword(s):  
Solar Wind ◽  
Solar Wind Turbulence ◽  
Wind Turbulence
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