Dominant two-dimensional solar wind turbulence with implications for cosmic ray transport

1996 ◽  
Vol 101 (A2) ◽  
pp. 2511-2522 ◽  
Author(s):  
John W. Bieber ◽  
Wolfgang Wanner ◽  
William H. Matthaeus
Keyword(s):  
Solar Wind ◽  
Cosmic Ray ◽  
Two Dimensional ◽  
Solar Wind Turbulence ◽  
Wind Turbulence

scholarly journals Three-dimensional spatial structures of solar wind turbulence from 10 000-km to 100-km scales

2011 ◽  
Vol 29 (10) ◽  
pp. 1731-1738 ◽  
Author(s):  
Y. Narita ◽  
K.-H. Glassmeier ◽  
M. L. Goldstein ◽  
U. Motschmann ◽  
F. Sahraoui
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Spatial Scales ◽  
Three Dimensional ◽  
Magnetic Field Direction ◽  
Two Dimensional ◽  
Solar Wind Turbulence ◽  
Symmetry Properties ◽  
Wind Turbulence ◽  
The Mean

Abstract. Using the four Cluster spacecraft, we have determined the three-dimensional wave-vector spectra of fluctuating magnetic fields in the solar wind. Three different solar wind intervals of Cluster data are investigated for this purpose, representing three different spatial scales: 10 000 km, 1000 km, and 100 km. The spectra are determined using the wave telescope technique (k-filtering technique) without assuming the validity of Taylor's frozen-in-flow hypothesis nor are any assumptions made as to the symmetry properties of the fluctuations. We find that the spectra are anisotropic on all the three scales and the power is extended primarily in the directions perpendicular to the mean magnetic field, as might be expected of two-dimensional turbulence, however, the analyzed fluctuations are not axisymmetric. The lack of axisymmetry invalidates some earlier techniques using single spacecraft observations that were used to estimate the percentage of magnetic energy residing in quasi-two-dimensional power. However, the dominance of two-dimensional turbulence is consistent with the relatively long mean free paths of cosmic rays in observed in the heliosphere. On the other hand, the spectra also exhibit secondary extended structures oblique from the mean magnetic field direction. We discuss possible origins of anisotropy and asymmetry of solar wind turbulence spectra.

scholarly journals Kinetic cascade beyond magnetohydrodynamics of solar wind turbulence in two-dimensional hybrid simulations

2012 ◽  
Vol 19 (2) ◽  
pp. 022305 ◽  
Author(s):  
D. Verscharen ◽  
E. Marsch ◽  
U. Motschmann ◽  
J. Müller
Keyword(s):  
Solar Wind ◽  
Two Dimensional ◽  
Solar Wind Turbulence ◽  
Wind Turbulence ◽  
Hybrid Simulations

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

scholarly journals Kinetic Cascade in Solar-wind Turbulence: 3D3V Hybrid-kinetic Simulations with Electron Inertia

2017 ◽  
Vol 846 (2) ◽  
pp. L18 ◽  
Author(s):  
Silvio Sergio Cerri ◽  
Sergio Servidio ◽  
Francesco Califano
Keyword(s):  
Solar Wind ◽  
Electron Inertia ◽  
Solar Wind Turbulence ◽  
Wind Turbulence

scholarly journals Solar Wind Turbulence from 1 to 45 au. IV. Turbulent Transport and Heating of the Solar Wind Using Voyager Observations

2020 ◽  
Vol 900 (2) ◽  
pp. 94 ◽  
Author(s):  
Zackary B. Pine ◽  
Charles W. Smith ◽  
Sophia J. Hollick ◽  
Matthew R. Argall ◽  
Bernard J. Vasquez ◽  
...  
Keyword(s):  
Solar Wind ◽  
Turbulent Transport ◽  
Solar Wind Turbulence ◽  
Wind Turbulence
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