Dissipation-Scale Turbulence in the Solar Wind

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dc.creatorHowes, Gregory G.
dc.creatorCowley, Steven C.
dc.creatorDorland, William
dc.creatorHammett, Gregory W.
dc.creatorQuataert, Eliot
dc.creatorSchekochihin, Alexander A.
dc.date2007-07-20
dc.date.accessioned2026-07-07T10:36:18Z
dc.date.available2026-07-07T10:36:18Z
dc.descriptionWe present a cascade model for turbulence in weakly collisional plasmas that follows the nonlinear cascade of energy from the large scales of driving in the MHD regime to the small scales of the kinetic Alfven wave regime where the turbulence is dissipated by kinetic processes. Steady-state solutions of the model for the slow solar wind yield three conclusions: (1) beyond the observed break in the magnetic energy spectrum, one expects an exponential cut-off; (2) the widely held interpretation that this dissipation range obeys power-law behavior is an artifact of instrumental sensitivity limitations; and, (3) over the range of parameters relevant to the solar wind, the observed variation of dissipation range spectral indices from -2 to -4 is naturally explained by the varying effectiveness of Landau damping, from an undamped prediction of -7/3 to a strongly damped index around -4.
dc.description6 pages, 2 figures, accepted for publication in AIP Conference Proceedings on "Turbulence and Nonlinear Processes in Astrophysical Plasmas"
dc.identifierhttps://arxiv.org/abs/0707.3149
dc.identifierhttp://arxiv.org/abs/0707.3149
dc.identifierAIPConf.Proc.932:3-8,2007
dc.identifierdoi:10.1063/1.2778938
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/180009
dc.subjectAstrophysics
dc.titleDissipation-Scale Turbulence in the Solar Wind
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