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.
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