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Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/2666
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dc.contributor.authorKrishan, V-
dc.contributor.authorSreedharan, T. D-
dc.contributor.authorMahajan, Swadesh M-
dc.date.accessioned2008-07-14T06:42:31Z-
dc.date.available2008-07-14T06:42:31Z-
dc.date.issued1991-04-
dc.identifier.citationMonthly Notices of Royal Astronomical Society, Vol. 249,No.4, pp. 596 - 601en
dc.identifier.issn0035-8711-
dc.identifier.urihttp://hdl.handle.net/2248/2666-
dc.description.abstractA Vlasov-Maxwell description of the ubiquitous solar coronal structures is presented. It is found that an equilibrium plasma configuration can live with spatial gradients in density, temperature, current and drift speeds of the charged particles. Any stability study must be carried out over this inhomogeneous equilibrium state. In addition, the Vlasov description admits the investigation of kinetic processes like heating and radiation and unlike a fluid description, it does not require an equation of state to determine the individual variations of temperature and density.en
dc.format.extent693951 bytes-
dc.format.mimetypeapplication/pdf-
dc.language.isoenen
dc.publisherRoyal Astronomical Societyen
dc.relation.urihttp://adsabs.harvard.edu/abs/1991MNRAS.249..596Ken
dc.subjectCoronal loopsen
dc.subjectMaxwell equationen
dc.subjectPlasma equilibriumen
dc.subjectSolar coronaen
dc.subjectVlasov equationsen
dc.subjectDensity distributionen
dc.subjectSolar temperatureen
dc.subjectTemperature distributionen
dc.titleVlasov-Maxwell equilibria of solar coronal loopsen
dc.typeArticleen
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