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Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/4162
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dc.contributor.authorSastry, Ch. V-
dc.contributor.authorDwarakanath, K. S-
dc.contributor.authorShevgaonkar, R. K-
dc.contributor.authorKrishan, V-
dc.date.accessioned2008-12-23T15:14:09Z-
dc.date.available2008-12-23T15:14:09Z-
dc.date.issued1981-10-
dc.identifier.citationSolar Physics, Vol. 73, No. 2, pp. 363 - 377en
dc.identifier.issn0038-0938-
dc.identifier.urihttp://hdl.handle.net/2248/4162-
dc.description.abstractWe have observed the slowly varying component of solar radio emission at a frequency of 34.5 MHz with half power beam widths of 26/40 in the east-west and north-south directions, respectively. It is found that the observed brightness temperatures vary within the limits of 0.3×106K to 1.5×106K, and the average half power widths of the brightness distribution on the Sun is about 3R . Thermal emission from coronal regions of various electron densities and temperatures with and without the magnetic field has been computed and compared with the observed results.en
dc.language.isoenen
dc.publisherD. Reidel Publishing Co.en
dc.relation.urihttp://dx.doi.org/10.1007/BF00151687en
dc.relation.urihttp://adsabs.harvard.edu/abs/1981SoPh...73..363Sen
dc.subjectBrightness Temperatureen
dc.subjectDecametric Wavesen
dc.subjectRadio Astronomyen
dc.subjectSolar Radio Emissionen
dc.subjectBrightness Distributionen
dc.subjectElectron Density (Concentration)en
dc.subjectElectron Energyen
dc.subjectSolar Coronaen
dc.subjectSolar Magnetic Fielden
dc.subjectThermal Emissionen
dc.titleObservations and interpretation of the slowly varying component of solar radio emission at decameter wavelengthsen
dc.typeArticleen
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