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

Y. Narita, K.-H. Glassmeier, F. Sahraoui, and M. L. Goldstein
Phys. Rev. Lett. 104, 171101 – Published 28 April 2010
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Abstract

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|1.5×103rad/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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  • Received 31 January 2008

DOI:https://doi.org/10.1103/PhysRevLett.104.171101

©2010 American Physical Society

Authors & Affiliations

Y. Narita* and K.-H. Glassmeier

  • Institut für Geophysik und extraterrestrische Physik, Technische Universität Braunschweig, Mendelssohnstraße 3, D-38106 Braunschweig, Germany

F. Sahraoui and M. L. Goldstein

  • Geospace Physics Laboratory, NASA Goddard Space Flight Center, Code 673, Greenbelt, Maryland 20771, USA

  • *y.narita@tu-bs.de
  • Also at: Max-Planck-Institut für Sonnensystemforschung, Max-Planck-Straße 2, D-37191 Katlenburg-Lindau, Germany.
  • Now at: Laboratoire de Physique des Plasmas, CNRS-Ecole Polytechnique, Vélizy, 78140, France.

See Also

Mapping Turbulence in the Solar Wind

Don Monroe
Phys. Rev. Focus 25, 16 (2010)

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Vol. 104, Iss. 17 — 30 April 2010

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