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Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/2709
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dc.contributor.authorDikpati, M-
dc.contributor.authorChoudhuri, A. R-
dc.date.accessioned2008-07-16T06:36:48Z-
dc.date.available2008-07-16T06:36:48Z-
dc.date.issued1996-03-
dc.identifier.citationAstrophysics and Space Science, Vol. 243, No.1, pp. 169 - 172en
dc.identifier.issn0004-640X-
dc.identifier.urihttp://hdl.handle.net/2248/2709-
dc.description.abstractWe assume the large-scale diffuse magnetic field of the Sun to originate from the poloidal component of a dynamo operating at the base of the convection zone, whereas the sunspots are due to the toroidal component. The evolution of the poloidal component is studied to model the poleward migration of the diffuse field seen on the solar surface and the polar reversal at the time of sunspots maxima (Dikpati and Choudhuri 1994, 1995).en
dc.format.extent332466 bytes-
dc.format.mimetypeapplication/pdf-
dc.language.isoenen
dc.publisherKluwer Academic Publishersen
dc.relation.urihttp://adsabs.harvard.edu/abs/1996Ap%26SS.243..169Den
dc.relation.urihttp://www.springerlink.com/content/u78p164358616632/en
dc.subjectSunspotsen
dc.subjectSolar magnetic fielden
dc.subjectPoloidal fielden
dc.titleOn the Out of Phase Appearance of Large-Scale Diffuse Magnetic Field of the Sun with Respect to Sunspotsen
dc.typeArticleen
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