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Non Axi-symmetric Anisotropy of Solar Wind Turbulence

dc.contributor.authorTurner, A. J.en_US
dc.contributor.authorGogoberidze, G.en_US
dc.contributor.authorChapman, S. C.en_US
dc.contributor.authorHnat, B.en_US
dc.contributor.authorMueller, W. -Cen_US
dc.date.accessioned2014-03-12T19:21:03Z
dc.date.available2014-03-12T19:21:03Z
dc.date.issued2011-8/2011en_US
dc.description.abstractA key prediction of turbulence theories is frame-invariance, and in magnetohydrodynamic (MHD) turbulence, axisymmetry of fluctuations with respect to the background magnetic field. Paradoxically the power in fluctuations in the turbulent solar wind are observed to be ordered with respect to the bulk macroscopic flow as well as the background magnetic field. Here, non- axisymmetry across the inertial and dissipation ranges is quantified using in-situ observations from Cluster. The observed inertial range non- axisymmetry is reproduced by a 'fly through' sampling of a Direct Numerical Simulation of MHD turbulence. Furthermore, 'fly through' sampling of a linear superposition of transverse waves with axisymmetric fluctuations generates the trend in non- axisymmetry with power spectral exponent. The observed non-axisymmetric anisotropy may thus simply arise as a sampling effect related to Taylor's hypothesis and is not related to the plasma dynamics itself.en_US
dc.identifier.citationTurner, A. J., G. Gogoberidze, S. C. Chapman, B. Hnat, et al. 2011. "Non Axi-symmetric Anisotropy of Solar Wind Turbulence." 107(9)en_US
dc.identifier.issn0031-9007en_US
dc.identifier.issue9en_US
dc.identifier.startpageen_US
dc.identifier.urihttp://dx.doi.org/10.1103/PhysRevLett.107.095002en_US
dc.identifier.urihttp://hdl.handle.net/10222/45453
dc.identifier.volume107en_US
dc.titleNon Axi-symmetric Anisotropy of Solar Wind Turbulenceen_US
dc.title.alternativePhysical Review Lettersen_US
dc.typearticleen_US

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