Wave-Vector Dependence of Magnetic-Turbulence Spectra in the Solar Wind





Citation of Original Publication

Narita, Y., K.-H. Glassmeier, F. Sahraoui, and M. L. Goldstein. “Wave-Vector Dependence of Magnetic-Turbulence Spectra in the Solar Wind.” Physical Review Letters 104, no. 17 (April 28, 2010): 171101. https://doi.org/10.1103/PhysRevLett.104.171101.


This work was written as part of one of the author's official duties as an Employee of the United States Government and is therefore a work of the United States Government. In accordance with 17 U.S.C. 105, no copyright protection is available for such works under U.S. Law.
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Using four-point measurements of the Cluster spacecraft, the energy distribution was determined for magnetic field fluctuations in the solar wind directly in the three-dimensional wave-vector domain in the range |k|≤1.5×10 ⁻³ rad/km. The energy distribution exhibits anisotropic features characterized by a prominently extended structure perpendicular to the mean field preferring the ecliptic north direction and also by a moderately extended structure parallel to the mean field. From the three-dimensional energy distribution wave vector anisotropy is estimated with respect to directions parallel and perpendicular to the mean magnetic field, and the result suggests the dominance of quasi-two-dimensional turbulence toward smaller spatial scales.