@article{oai:nagoya.repo.nii.ac.jp:00019897,
 author = {KAKINUMA, Takakiyo and ENOME, Shinzo},
 journal = {Proceedings of the Research Institute of Atmospherics, Nagoya University},
 month = {Mar},
 note = {The new 32+2-element interferometer at 9.4 Gc/s was completed in June 1966. Observations are being carried out every day for two hours, before and after the local noon, mainly with 1.1 min. of arc beams. Two or three drift-curves near local noon are taken with 21 sec. of arc beams. On September 21, 1966, an impulsive burst was observed on a frequency range from 1 Gc/s to 9. 4 Gc/s. The source of this burst had a bipolar structure, that is, the source consisted of two separated polarized regions each having an opposite sense of polarization. The source of burst seems to be confined in the small (＜1') regions of strong magnetic field over each pole of the bipolar sunspot group. On July 29, 1966, the source of the long enduring burst was observed. The position of the radio emissive region corresponded to that of the flare and the size of the region was 2 min. of arc. The time-variation of radio spectra suggests that the burst exhibits thermal spectra in the declining phase. The electron temperature and the so-called emission measure of the region are estimated to be 3×10^6 K and 10^-29 cm^-5 respectively.},
 pages = {23--34},
 title = {HIGH-RESOLUTION OBSERVATIONS OF THE SOURCES OF SOLAR RADIO BURST AT 9. 4 GC/S.},
 volume = {14},
 year = {1967}
}