Anisotropy of the Taylor scale and the correlation scale in plasma sheet and solar wind magnetic field fluctuations

Details Anisotropy of the Taylor scale and the correlation scale in plasma sheet and solar wind magnetic field fluctuations Anisotropy of the Taylor scale and the correlation scale in plasma sheet and solar wind magnetic field fluctuations

Jul 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009jgra..11407213w&link_type=abstract

Journal of Geophysical Research, Volume 114, Issue A7, CiteID A07213

Physics

Plasma Physics

18

Space Plasma Physics: Turbulence (4490), Magnetospheric Physics: Plasma Sheet, Magnetospheric Physics: Solar Wind Interactions With Unmagnetized Bodies, Nonlinear Geophysics (3200, 6944, 7839)

Scientific paper

Magnetic field data from nine spacecraft in the magnetospheric plasma sheet and the solar wind are employed to determine the correlation scale and the magnetic Taylor microscale from simultaneous multiple-point measurements for multiple intervals with a range of mean magnetic field directions. We have determined that in the solar wind the Taylor scale is independent of direction relative to the mean magnetic field, but the correlation scale along the mean magnetic field (2.7 × 106 ± 0.2 × 106 km) is longer than along the perpendicular direction (1.5 × 106 ± 0.1 × 106 km). Within the plasma sheet we found that the correlation scale varies from 16,400 ± 1000 km along the mean magnetic field direction to 9200 ± 600 km in the perpendicular direction. The Taylor scale is also longer parallel to the magnetic field (2900 ± 100 km) than perpendicular to it (1100 ± 100 km). In the solar wind the ratio of the parallel correlation scale to the perpendicular correlation scale is 2.62 ± 0.79; in the plasma sheet the ratio is 1.78 ± 0.16, which indicates that the turbulence in both regions is anisotropic. The correlation and Taylor scales may be used to estimate effective magnetic Reynolds numbers separately for each angular channel. Reynolds numbers were found to be approximately independent of the angle relative to the mean magnetic field. These results may be useful in magnetohydrodynamic modeling of the solar wind and the magnetosphere and can contribute to our understanding of solar and galactic cosmic ray diffusion in the heliosphere.

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