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Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/2434
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dc.contributor.authorSreedharan, T. D-
dc.contributor.authorSasidharan, K-
dc.contributor.authorSatya Narayanan, A-
dc.contributor.authorKrishan, V-
dc.date.accessioned2008-06-16T09:11:17Z-
dc.date.available2008-06-16T09:11:17Z-
dc.date.issued1992-12-
dc.identifier.citationSolar Physics, Vol. 142, No. 2, pp. 249 - 264en
dc.identifier.urihttp://hdl.handle.net/2248/2434-
dc.description.abstractThe theory of ideal magnetohydrodynamic turbulence in cylindrical geometry is used to study the steady-state structure of a coronal loop. The pressure profile is derived from MHD equations by representing the velocity and magnetic fields as the superposition of Chandrasekhar-Kendall functions. Such a representation brings out the three-dimensional structure of the pressure in the coronal loop. The radial, azimuthal, and axial variations of the pressure for a constant density loop are discussed in detail. The pressure has an oscillatory behavior for different azimuthal angles at some radial positions. This study predicts more features in pressure than can be compared with the presently available observations.en
dc.format.extent1143886 bytes-
dc.format.mimetypeapplication/pdf-
dc.language.isoenen
dc.publisherSpringer Netherlandsen
dc.relation.urihttp://www.springerlink.com/content/l467w85015167455/en
dc.relation.urihttp://adsabs.harvard.edu/abs/1992SoPh..142..249Sen
dc.subjectSolar Coronaen
dc.subjectSolar activityen
dc.subjectsolar magnetic fielden
dc.titlePressure structure of solar coronal loops. IIIen
dc.typeArticleen
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