Scale invariance of normalized cross-helicity throughout the inertial range of solar wind turbulence

2010 ◽  
Vol 17 (11) ◽  
pp. 112905 ◽  
Author(s):  
J. J. Podesta ◽  
J. E. Borovsky
Keyword(s):  
Solar Wind ◽  
Scale Invariance ◽  
Inertial Range ◽  
Solar Wind Turbulence ◽  
Wind Turbulence

scholarly journals ENHANCED MAGNETIC COMPRESSIBILITY AND ISOTROPIC SCALE INVARIANCE AT SUB-ION LARMOR SCALES IN SOLAR WIND TURBULENCE

2012 ◽  
Vol 763 (1) ◽  
pp. 10 ◽  
Author(s):  
K. H. Kiyani ◽  
S. C. Chapman ◽  
F. Sahraoui ◽  
B. Hnat ◽  
O. Fauvarque ◽  
...  
Keyword(s):  
Solar Wind ◽  
Scale Invariance ◽  
Solar Wind Turbulence ◽  
Wind Turbulence

Statistical Research of the Intermittency and Cascade of Solar Wind Turbulence Based on Analysis of PSP Measurements

2020 ◽  
Author(s):  
Ying Wang ◽  
Jiansen He ◽  
Die Duan ◽  
Xingyu Zhu
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Break Point ◽  
Inertial Range ◽  
Scaling Exponent ◽  
The Sun ◽  
Peak Point ◽  
Solar Wind Turbulence ◽  
Wind Turbulence ◽  
Inner Heliosphere

<p>By analyzing the turbulent magnetic field data from PSP, we find that: the solar wind turbulence in the inner heliosphere close to the Sun has formed the transition from multifractal intermittency at MHD scales to monofractal intermittency at kinetic scales. The order-dependent scaling exponent of the multi-order structure function shows a concave profile indicating the multifractal property at MHD scales, while its counterpart at kinetic scales shows a linear trend suggesting the monofractal property. We also find that, the closer to the sun, the more obvious the concave profile of the scaling exponent in the inertial range, which indicates that the multifractal characteristic of the magnetic field turbulence intermittency is also more evident when getting closer to the Sun.</p><p>Based on the Castaing description of the probability distribution function(PDF) of the disturbance difference, the key parameters(μ & λ^2) of the Castaing function are estimated as a function of scale. We find that: (1) when close to the sun (R~0.17 AU), the break point of μ is about 0.2 second, and the peak point of λ^2 is about 0.6 second, the two of which are about three times different in scale; (2) when far from the sun (R~0.8 AU), the break point of μ is about 1 second and the peak point of λ^2 is about 3 seconds, the two of which are also about three times different in scale. We also point out that the profiles (including the break/peak position) of both the parameters (μ & λ^2) along with the scale together determine the profile (including the spectral breaks) of the power spectrum.</p><p>Following the PP98 model function of incompressible MHD turbulent cascade rate (εZ), we first compared the cascade rate εZ with εB=<δB^3>/τ at the distance close to the sun, we find that the two trends over scales are in good agreement with one another. We therefore suggest that, to some extent (e.g. in the inertial region), εB=<δB^3>/τ can be used as a proxy of the cascade rate εZ. For the first time, by statistical analysis, we obtained that εB satisfies the following relation with the scale and the heliocentric distance: εB=((τ/τ0)^α)((r/r0)^β). In the inertial range, α changes from about -0.5 to about 0.5 as r increases from 0.17 AU to 0.81 AU, and β is about 6.4; in the kenetic range, when r increases from 0.17 AU to 0.25 AU, α keeps at about 2, and β is about 12.8. The εB(τ,r) expression given in this work, is believed to help understanding the transport and cascade processes of solar wind turbulence in the inner heliosphere. </p><p>Corresponding author:<br>Jiansen HE, [email protected]</p><p>Acknowledgements:<br>We would like to thank the PSP team for providing the data of PSP to the public.</p>

scholarly journals Dependence of 3D Self-correlation Level Contours on the Scales in the Inertial Range of Solar Wind Turbulence

2019 ◽  
Vol 883 (1) ◽  
pp. L9 ◽  
Author(s):  
Honghong Wu ◽  
Chuanyi Tu ◽  
Xin Wang ◽  
Jiansen He ◽  
Linghua Wang
Keyword(s):  
Solar Wind ◽  
Inertial Range ◽  
Solar Wind Turbulence ◽  
Wind Turbulence ◽  
Correlation Level

scholarly journals Solar Wind Turbulence from 1 to 45 au. II. Analysis of Inertial-range Fluctuations Using Voyager and ACE Observations

2020 ◽  
Vol 900 (2) ◽  
pp. 92 ◽  
Author(s):  
Zackary B. Pine ◽  
Charles W. Smith ◽  
Sophia J. Hollick ◽  
Matthew R. Argall ◽  
Bernard J. Vasquez ◽  
...  
Keyword(s):  
Solar Wind ◽  
Inertial Range ◽  
Solar Wind Turbulence ◽  
Wind Turbulence

scholarly journals Solar Wind Turbulence from 1 to 45 au. III. Anisotropy of Magnetic Fluctuations in the Inertial Range Using Voyager and ACE Observations

2020 ◽  
Vol 900 (2) ◽  
pp. 93 ◽  
Author(s):  
Zackary B. Pine ◽  
Charles W. Smith ◽  
Sophia J. Hollick ◽  
Matthew R. Argall ◽  
Bernard J. Vasquez ◽  
...  
Keyword(s):  
Solar Wind ◽  
Inertial Range ◽  
Magnetic Fluctuations ◽  
Solar Wind Turbulence ◽  
Wind Turbulence

scholarly journals Spectral anisotropy of solar wind turbulence in the inertial range and dissipation range

2010 ◽  
Author(s):  
J. J. Podesta ◽  
M. Maksimovic ◽  
K. Issautier ◽  
N. Meyer-Vernet ◽  
M. Moncuquet ◽  
...  
Keyword(s):  
Solar Wind ◽  
Inertial Range ◽  
Solar Wind Turbulence ◽  
Wind Turbulence ◽  
Dissipation Range
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