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Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/2244
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dc.contributor.authorPandey, K-
dc.contributor.authorNarain, U-
dc.date.accessioned2008-04-22T07:11:04Z-
dc.date.available2008-04-22T07:11:04Z-
dc.date.issued2001-
dc.identifier.citationBASI, Vol. 29, No. 3, pp. 231 - 238en
dc.identifier.urihttp://hdl.handle.net/2248/2244-
dc.description.abstractWe review heating of solar corona by magnetic fields/currents. Our emphasis is on micro- and nano-flares. In case of a microflare the energy release is ~1026 ergs whereas in a nanoflare ~1023 - 1025 ergs of energy is released. Flares have a distribution law over total radiated energy with exponent α = 1.8. Extending the same power law to micro-and nano-flares and assuming that they constitute a dominant heating mechanism for solar corona ??must be greater than 2. Many investigations lead to α < 2 whereas a few yield α > 2. The verdict remains inconclusive. More observational analyses and numerical simulations are needed to discriminate between the two cases.en
dc.format.extent653694 bytes-
dc.format.mimetypeapplication/pdf-
dc.language.isoenen
dc.publisherAstronomical Society of Indiaen
dc.relation.urihttp://adsabs.harvard.edu/abs/2001BASI...29..231Pen
dc.subjectCoronal heatingen
dc.subjectSolar coronaen
dc.titleOn solar coronal heatingen
dc.typeArticleen
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