@article{oai:nagoya.repo.nii.ac.jp:00019413,
 author = {TANAKA, HARUO and KAKINUMA, TAKAKIYO},
 journal = {Proceedings of the Research Institute of Atmospherics, Nagoya University},
 month = {Mar},
 note = {With the intention of locating sources of solar noise at 4,000 MC, an interferometer with 5 aerials has been constructed. Each aerial has a paraboloidal reflector of size 1.5 meter in diameter, which can automatically follow the sun. Aerials are placed in E-W direction at 6 metre intervals. The main lobes are 43' apart and have half-power widths of 7.8'. The output of each aerial is connected with waveguides and magic Tees and is led into the radiometer. General design principles and results of observations are described in this paper. From the eclipse observations on Feb. 14, 1953, it is concluded that the radio disk of the sun is about 1.06 times larger than the optical one. In associated with the record of interferometer, we supposed a simple model about the radio distribution on the quiet solar disk, that is, the 6% excess region is 2.5 times brighter than the optical disk of the uniform temperature of 1.9x10^4 degree K. The aerials of the interferometer are expected to be increased to 8-element in spring, 1954. At the same time, quarter-wavelength plates will be set up for the observation of polarized waves.},
 pages = {53--76},
 title = {MULTIPLE ELEMENT INTERFEROMETER FOR LOCATING SOURCES OF SOLAR NOISE AT 4,000 MEGACYCLES (I)},
 volume = {2},
 year = {1954}
}