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

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

Apr 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010phrvl.104q1101n&link_type=abstract

Physical Review Letters, vol. 104, Issue 17, id. 171101

Physics

15

Solar Wind Plasma, Sources Of Solar Wind, Plasma Turbulence

Scientific paper

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|≤1.5×10-3rad/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.

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