Abstract
With the intention of locating sources of radio noise from the disturbed sun at 4,000 MC, an interferometer with 5 aerials was constructed. Each aerial has a paraboloidal reflector of size 1.5 metre in diameter, which can be rotated equatorially. They are placed in E-W direction at 6 m intervals. The main lobes are 43' apart and each lobe has a half power width of 7.8'. Each aerial is connected to the radiometer with waveguides and magic T . General design principles and the results of observations are described in this paper. Experimental record pattern, when the sun is quiet, do not agree with the calculated one corresponding to uniform distribution over the optical disk. From the eclipse observation, it is concluded that the radio disk is about 1.06 times larger than the optical disk. Record pattern is obtained if the outer region is about 2.5 times brighter than the optical disk of the uniform temperature about 1.9×10 4 °K.
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