Anisotropy of Solar Wind Turbulence in the Dissipation Range

Details Anisotropy of Solar Wind Turbulence in the Dissipation Range Anisotropy of Solar Wind Turbulence in the Dissipation Range

Dec 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufmsh51c..08c&link_type=abstract

American Geophysical Union, Fall Meeting 2009, abstract #SH51C-08

Physics

Plasma Physics

[2159] Interplanetary Physics / Plasma Waves And Turbulence, [2164] Interplanetary Physics / Solar Wind Plasma, [7863] Space Plasma Physics / Turbulence

Scientific paper

Although turbulence is readily observed in the solar wind, some aspects are poorly understood with unexplained observations and conflicting theoretical descriptions. In particular the dissipation range (fluctuations smaller than the ion gyroscale) is only just beginning to be thoroughly investigated. Here we present methods and results from a multi-spacecraft analysis of the solar wind dissipation range between the ion and electron gyroscales using the four Cluster satellites. We find that the fluctuations are anisotropic, having a higher power in the direction perpendicular to the local mean magnetic field than parallel to it. We also compare the observed anisotropic scaling to predictions for a kinetic Alfven wave cascade. The implications of anisotropic fluctuations for the interpretation of dissipation range measurements in general are also discussed.

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