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Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/1888
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dc.contributor.authorVats, H. O-
dc.contributor.authorDeshpande, M. R-
dc.contributor.authorMehta, M-
dc.contributor.authorShah, C. R-
dc.contributor.authorShah, K. J-
dc.date.accessioned2007-10-16T09:27:26Z-
dc.date.available2007-10-16T09:27:26Z-
dc.date.issued1999-
dc.identifier.citationBASI, Vol. 27, No. 1, pp. 61 - 63en
dc.identifier.urihttp://hdl.handle.net/2248/1888-
dc.description.abstractThe time series of solar radio emission at 2.8 GHz is analysed using correlation methods. The analysis showed that this type of time series can be used to infer the rotation period of the source (in this case solar corona). It is found that the correlograms have a very strong persistence of rotational modulation. These values are significantly lower than those reported earlier by other methods. The reasons for this difference are unknown.en
dc.format.extent256748 bytes-
dc.format.mimetypeapplication/pdf-
dc.language.isoenen
dc.publisherAstronomical Society of Indiaen
dc.relation.urihttp://adsabs.harvard.edu/abs/1999BASI...27...61Ven
dc.subjectRadio emissionen
dc.subjectSolar radio emissionen
dc.subjectCoronal rotationen
dc.titleRadio emission as a diagnostic for solar coronal rotationen
dc.typeArticleen
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