Turbulence in the Solar Corona

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dc.creatorCranmer, Steven R.
dc.date2007-06-19
dc.date.accessioned2026-07-07T10:36:10Z
dc.date.available2026-07-07T10:36:10Z
dc.descriptionThe solar corona has been revealed in the past decade to be a highly dynamic nonequilibrium plasma environment. Both the loop-filled coronal base and the extended acceleration region of the solar wind appear to be strongly turbulent, but direct observational evidence for a cascade of fluctuation energy from large to small scales is lacking. In this paper I will review the observations of wavelike motions in the corona over a wide range of scales, as well as the macroscopic effects of wave-particle interactions such as preferential ion heating. I will also present a summary of recent theoretical modeling efforts that seem to explain the time-steady properties of the corona (and the fast and slow solar wind) in terms of an anisotropic MHD cascade driven by the partial reflection of low-frequency Alfven waves propagating along the superradially expanding solar magnetic field. Complete theoretical models are difficult to construct, though, because many of the proposed physical processes act on a multiplicity of spatial scales (from centimeters to solar radii) with feedback effects not yet well understood. This paper is thus a progress report on various attempts to couple these disparate scales.
dc.description6 pages, 1 figure (AIP 6x9 style), to appear in AIP Conference Proceedings: "Turbulence and Nonlinear Processes in Astrophysical Plasmas" (6th Annual IGPP International Astrophysics Conference), Waikiki, March 16-22, 2007
dc.identifierhttps://arxiv.org/abs/0706.2843
dc.identifierhttp://arxiv.org/abs/0706.2843
dc.identifierAIPConf.Proc.932:271-276,2007
dc.identifierdoi:10.1063/1.2778974
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/179963
dc.subjectAstrophysics
dc.titleTurbulence in the Solar Corona
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