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

Journal Article · Fri Apr 30 00:00:00 EDT 2010 · Physical Review Letters

DOI:https://doi.org/10.1103/PHYSREVLETT.104.171101· OSTI ID:21410657

Narita, Y; Glassmeier, K -H; Sahraoui, F; Goldstein, M L ^[1]

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1. Institut fuer Geophysik und extraterrestrische Physik, Technische Universitaet Braunschweig, Mendelssohnstrasse 3, D-38106 Braunschweig (Germany)

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|{<=}1.5x10{sup -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.

• OSTI ID: 21410657
• Journal Information: Physical Review Letters, Vol. 104, Issue 17; Other Information: DOI: 10.1103/PhysRevLett.104.171101; (c) 2010 The American Physical Society; ISSN 0031-9007
• Country of Publication: United States
• Language: English

Related Subjects

70 PLASMA PHYSICS AND FUSION TECHNOLOGY
ANISOTROPY
ENERGY SPECTRA
FLUCTUATIONS
MAGNETIC FIELDS
MEAN-FIELD THEORY
RADIATION DOSE UNITS
SOLAR WIND
SPACE VEHICLES
THREE-DIMENSIONAL CALCULATIONS
TURBULENCE
TWO-DIMENSIONAL CALCULATIONS
VECTORS
SOLAR ACTIVITY
SPECTRA
STELLAR ACTIVITY
STELLAR WINDS
TENSORS
UNITS
VARIATIONS
VEHICLES