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Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/3471
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dc.contributor.authorVerma, M. K-
dc.date.accessioned2008-09-08T14:22:35Z-
dc.date.available2008-09-08T14:22:35Z-
dc.date.issued1998-
dc.identifier.citationBASI, Vol. 26, pp. 231 - 232en
dc.identifier.urihttp://hdl.handle.net/2248/3471-
dc.description.abstractAlfvenic fluctuations in the solar wind is known to exhibit turbulent behaviour. In this paper we state the existing phenomenologies. After this we show the numerical results from pseudo-spectral method. The numerical results appear to favour the Kolmogorov-like MHD turbulence phenomenology over the Kraichnan phenomenology atleast in some regime.en
dc.language.isoenen
dc.publisherAstronomical Society of Indiaen
dc.relation.urihttp://adsabs.harvard.edu/abs/1998BASI...26..231Ven
dc.subjectSolar winden
dc.subjectTurbulenceen
dc.subjectDissipationen
dc.titleMagnetohydrodynamic turbulence in solar winden
dc.typeArticleen
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