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Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/3230
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dc.contributor.authorKrishan, V-
dc.date.accessioned2008-08-22T05:29:35Z-
dc.date.available2008-08-22T05:29:35Z-
dc.date.issued1997-07-
dc.identifier.citationPramana - Journal of Physics, Vol. 49, No. 1, pp. 147 - 154en
dc.identifier.issn0304-4289-
dc.identifier.urihttp://hdl.handle.net/2248/3230-
dc.description.abstractThe rotation curves of galaxies are modelled using very special properties of an hydrodynamically turbulent fluid possessing helicity fluctuations. The development of correlations among these fluctuations leads to the formation of organized structures characterized by a new flat branch of the spatial energy spectrum in addition to the well known Kolmogorov spectrum. It is proposed that the flat nature of the rotation curves of galaxies may be a result of the energy cascading processes occurring in turbulent galactic atmospheres. Thus, in this model, there is no need of invoking dark matter to account for the flat rotation curves of galaxies.en
dc.format.extent89728 bytes-
dc.format.mimetypeapplication/pdf-
dc.language.isoenen
dc.publisherIndian Academy of Scienceen
dc.relation.urihttp://adsabs.harvard.edu/abs/1997Prama..49..147Ken
dc.relation.urihttp://www.springerlink.com/content/v64h1174l4014811/-
dc.subjectKolmogorov Theoryen
dc.subjectGalaxiesen
dc.subjectAstrophysicsen
dc.subjectMathematical Modelsen
dc.subjectCorrelationen
dc.subjectTurbulenceen
dc.subjectFluid Mechanicsen
dc.subjectHydrodynamicsen
dc.subjectSpectrum Analysisen
dc.subjectAtmosphericsen
dc.titleRotation curves of galaxies: missing mass or missing physicsen
dc.typeArticleen
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