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Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/4929
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dc.contributor.authorKrishan, V-
dc.contributor.authorBerger, M-
dc.contributor.authorPriest, E. R-
dc.date.accessioned2009-12-03T11:15:09Z-
dc.date.available2009-12-03T11:15:09Z-
dc.date.issued1988-07-
dc.identifier.citationAltrock, Richard C. ed., Solar and stellar coronal structure and dynamics:A Festschrift in honor of Dr. John W-Evans: Proceedings of the Ninth Sacramento Peak Summer Symposium, Sunspot, NM 17 - 21, August, 1987, pp. 236 - 247en
dc.identifier.urihttp://hdl.handle.net/2248/4929-
dc.description.abstractThe coronal loop plasma is represented by a superposition of the three lowest order Chandrasekhar-Kendall modes. The temporal evolution of the velocity and magnetic field in each of these mode is determined using ideal MHD equations under two simplified cases viz (i) allowing small departures from the equilibrium and (ii) the pump approximation.en
dc.language.isoenen
dc.publisherNational Solar Observatoryen
dc.rights© National Solar Observatoryen
dc.subjectDynamicsen
dc.subjectMagnetic and Velocity Fieldsen
dc.subjectCoronal Loopsen
dc.subjectSolar Physicsen
dc.subjectSolar Coronaen
dc.titleDynamics of magnetic and velocity fields in coronal loopsen
dc.typeArticleen
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