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Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/4243
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dc.contributor.authorGopalswamy, N-
dc.contributor.authorThejappa, G-
dc.contributor.authorSastry, Ch. V-
dc.contributor.authorTlamicha, A-
dc.date.accessioned2009-01-07T12:27:09Z-
dc.date.available2009-01-07T12:27:09Z-
dc.date.issued1986-03-
dc.identifier.citationBulletin of Astronomical Institutes of Czechoslovakia, Vol. 37, pp. 115 - 120en
dc.identifier.issn0004-6248-
dc.identifier.urihttp://hdl.handle.net/2248/4243-
dc.description.abstractThe radial dependence of the coronal magnetic field above active regions is calculated using Type-I chain data existing in the literature. Assuming that Type-I emission is due to shock waves, the upstream shock velocity and the density jump across the shock are obtained respectively from the drift rate and the bandwidth of the Type-I chains. Making use of the shock velocity and the density jump in the Rankine-Hugoniot relation, the Alfvén velocity and hence the magnetic field in the corona is calculated. The results are compared with existing estimates.en
dc.language.isoenen
dc.publisherCzechoslovakia Academy of Sciencesen
dc.relation.urihttp://adsabs.harvard.edu/abs/1986BAICz..37..115Gen
dc.subjectCoronal Loopsen
dc.subjectSolar Coronaen
dc.subjectSolar Magnetic Fielden
dc.subjectSolar Radio Burstsen
dc.subjectPropagation Velocityen
dc.subjectRankine-Hugoniot Relationen
dc.subjectShock Wave Propagationen
dc.subjectSolar Activityen
dc.titleEstimation of coronal magnetic fields using Type-I emissionen
dc.typeArticleen
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