Kolmogorov and Irosnikov-Kraichnan scaling in the anisotropic turbulent solar wind

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dc.creatorChapman, S. C.
dc.creatorHnat, B.
dc.date2006-06-13
dc.date.accessioned2026-07-07T08:28:53Z
dc.date.available2026-07-07T08:28:53Z
dc.descriptionSolar wind turbulence is dominated by Alfvénic fluctuations but the power spectral exponents somewhat surprisingly evolve toward the Kolmogorov value of -5/3, that of hydrodynamic turbulence. We show that at 1AU the turbulence decomposes linearly into two coexistent components perpendicular and parallel to the local average magnetic field. The first of these is consistent with propagating Alfvén wavepackets and shows the scaling expected of Alfvénic turbulence, namely Irosnikov- Kraichnan. The second shows Kolmogorov scaling which we also find in the number and magnetic energy density, and Poynting flux.
dc.description4 pages, 6 figures, submitted PRL
dc.identifierhttps://arxiv.org/abs/physics/0606106
dc.identifierhttp://arxiv.org/abs/physics/0606106
dc.identifierChapman, S. C., and B. Hnat (2007), Quantifying scaling in the velocity field of the anisotropic turbulent solar wind, Geophys. Res. Lett., 34, L17103
dc.identifierdoi:10.1029/2007GL030518
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/137775
dc.subjectPlasma Physics
dc.subjectFluid Dynamics
dc.titleKolmogorov and Irosnikov-Kraichnan scaling in the anisotropic turbulent solar wind
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