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Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/3536
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dc.contributor.authorVenkatakrishnan, P-
dc.date.accessioned2008-09-10T15:23:26Z-
dc.date.available2008-09-10T15:23:26Z-
dc.date.issued1990-
dc.identifier.citationIAU Symposium, No. 142, pp. 319 - 322en
dc.identifier.issn0074-1809-
dc.identifier.urihttp://hdl.handle.net/2248/3536-
dc.description.abstractMagnetic tension possesses low values at regions of large magnetic “shear” on the polarity inversion line. The low tension allows for a non-force-free field that depends on the density may then possibly evolve into solar flares. Heuristic arguments are given to favour instability driven flare scenarios.en
dc.language.isoenen
dc.publisherInternational Astronomical Unionen
dc.relation.urihttp://adsabs.harvard.edu/abs/1990IAUS..142..319Ven
dc.subjectMagnetic Shearen
dc.subjectFlaresen
dc.titleMagnetic Shear and Flaresen
dc.typeArticleen
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