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Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/2821
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dc.contributor.authorSubramanian, K-
dc.date.accessioned2008-07-22T11:44:33Z-
dc.date.available2008-07-22T11:44:33Z-
dc.date.issued2002-09-
dc.identifier.citationBASI, Vol. 30, No. 3, pp. 715 - 721en
dc.identifier.urihttp://hdl.handle.net/2248/2821-
dc.description.abstractMagnetic fields correlated on kiloparsec scales are seen in spiral galaxies. Their origin ~ould be due to amplification of a small seed field by a turbulent galactic dynamo. We review the current status of the galactic dynamo, especially the constraints imposed by magnetic helicity conservation. We estimate the minimal strength of the large-scale magnetic field which could arise in spite of the helicity constraint.en
dc.format.extent283038 bytes-
dc.format.mimetypeapplication/pdf-
dc.language.isoenen
dc.publisherAstronomical Society of Indiaen
dc.subjectGalaxiesen
dc.subjectGalactic Magnetic Fieldsen
dc.subjectDynamosen
dc.subjectMagnetic Helicityen
dc.titleMagnetic helicity in galactic dynamosen
dc.typeArticleen
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