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Title: THREE-DIMENSIONAL STRUCTURE OF SOLAR WIND TURBULENCE

Abstract

We present a measurement of the scale-dependent, three-dimensional structure of the magnetic field fluctuations in inertial range solar wind turbulence with respect to a local, physically motivated coordinate system. The Alfvenic fluctuations are three-dimensionally anisotropic, with the sense of this anisotropy varying from large to small scales. At the outer scale, the magnetic field correlations are longest in the local fluctuation direction, consistent with Alfven waves. At the proton gyroscale, they are longest along the local mean field direction and shortest in the direction perpendicular to the local mean field and the local field fluctuation. The compressive fluctuations are highly elongated along the local mean field direction, although axially symmetric perpendicular to it. Their large anisotropy may explain why they are not heavily damped in the solar wind.

Authors:
;  [1]; ;  [2];  [3];  [4]
  1. Space Sciences Laboratory, University of California, Berkeley, CA 94720 (United States)
  2. Rudolf Peierls Centre for Theoretical Physics, University of Oxford, Oxford OX1 3NP (United Kingdom)
  3. Blackett Laboratory, Imperial College London, London SW7 2AZ (United Kingdom)
  4. Heliophysics Science Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771 (United States)
Publication Date:
OSTI Identifier:
22086500
Resource Type:
Journal Article
Journal Name:
Astrophysical Journal
Additional Journal Information:
Journal Volume: 758; Journal Issue: 2; Other Information: Country of input: International Atomic Energy Agency (IAEA); Journal ID: ISSN 0004-637X
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ALFVEN WAVES; ANISOTROPY; ASTRONOMY; ASTROPHYSICS; AXIAL SYMMETRY; COORDINATES; CORRELATIONS; FLUCTUATIONS; MAGNETIC FIELDS; MAGNETOHYDRODYNAMICS; MEAN-FIELD THEORY; PLASMA; SOLAR PROTONS; SOLAR WIND; THREE-DIMENSIONAL CALCULATIONS; TURBULENCE

Citation Formats

Chen, C. H. K., Bale, S. D., Mallet, A., Schekochihin, A. A., Horbury, T. S., and Wicks, R. T., E-mail: chen@ssl.berkeley.edu. THREE-DIMENSIONAL STRUCTURE OF SOLAR WIND TURBULENCE. United States: N. p., 2012. Web. doi:10.1088/0004-637X/758/2/120.
Chen, C. H. K., Bale, S. D., Mallet, A., Schekochihin, A. A., Horbury, T. S., & Wicks, R. T., E-mail: chen@ssl.berkeley.edu. THREE-DIMENSIONAL STRUCTURE OF SOLAR WIND TURBULENCE. United States. doi:10.1088/0004-637X/758/2/120.
Chen, C. H. K., Bale, S. D., Mallet, A., Schekochihin, A. A., Horbury, T. S., and Wicks, R. T., E-mail: chen@ssl.berkeley.edu. Sat . "THREE-DIMENSIONAL STRUCTURE OF SOLAR WIND TURBULENCE". United States. doi:10.1088/0004-637X/758/2/120.
@article{osti_22086500,
title = {THREE-DIMENSIONAL STRUCTURE OF SOLAR WIND TURBULENCE},
author = {Chen, C. H. K. and Bale, S. D. and Mallet, A. and Schekochihin, A. A. and Horbury, T. S. and Wicks, R. T., E-mail: chen@ssl.berkeley.edu},
abstractNote = {We present a measurement of the scale-dependent, three-dimensional structure of the magnetic field fluctuations in inertial range solar wind turbulence with respect to a local, physically motivated coordinate system. The Alfvenic fluctuations are three-dimensionally anisotropic, with the sense of this anisotropy varying from large to small scales. At the outer scale, the magnetic field correlations are longest in the local fluctuation direction, consistent with Alfven waves. At the proton gyroscale, they are longest along the local mean field direction and shortest in the direction perpendicular to the local mean field and the local field fluctuation. The compressive fluctuations are highly elongated along the local mean field direction, although axially symmetric perpendicular to it. Their large anisotropy may explain why they are not heavily damped in the solar wind.},
doi = {10.1088/0004-637X/758/2/120},
journal = {Astrophysical Journal},
issn = {0004-637X},
number = 2,
volume = 758,
place = {United States},
year = {2012},
month = {10}
}