Observations and interpretation of the slowly varying component of solar radio emission at decameter wavelengths

Sastry, Ch. V; Dwarakanath, K. S; Shevgaonkar, R. K; Krishan, V

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dc.contributor.author	Sastry, Ch. V
dc.contributor.author	Dwarakanath, K. S
dc.contributor.author	Shevgaonkar, R. K
dc.contributor.author	Krishan, V
dc.date.accessioned	2008-12-23T15:14:09Z
dc.date.available	2008-12-23T15:14:09Z
dc.date.issued	1981-10
dc.identifier.citation	Solar Physics, Vol. 73, No. 2, pp. 363 - 377	en
dc.identifier.issn	0038-0938
dc.identifier.uri	http://hdl.handle.net/2248/4162
dc.description.abstract	We 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.iso	en	en
dc.publisher	D. Reidel Publishing Co.	en
dc.relation.uri	http://dx.doi.org/10.1007/BF00151687	en
dc.relation.uri	http://adsabs.harvard.edu/abs/1981SoPh...73..363S	en
dc.subject	Brightness Temperature	en
dc.subject	Decametric Waves	en
dc.subject	Radio Astronomy	en
dc.subject	Solar Radio Emission	en
dc.subject	Brightness Distribution	en
dc.subject	Electron Density (Concentration)	en
dc.subject	Electron Energy	en
dc.subject	Solar Corona	en
dc.subject	Solar Magnetic Field	en
dc.subject	Thermal Emission	en
dc.title	Observations and interpretation of the slowly varying component of solar radio emission at decameter wavelengths	en
dc.type	Article	en