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68. Polarization of solar radio bursts

  • T. Hatanaka (a1)

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The polarization observation of solar radio emission at 200 Mc./s. was started in December 1954 at the Tokyo Astronomical Observatory with a new type of radio polarimeter[1, 2]. With a pair of crossed dipoles at the focus of a 10 metre paraboloid of equatorial mounting, it gives almost simultaneously six components of polarization, two circular and four linear, on a time-sharing basis by using electronic switching. Fig. 1 shows the block diagram of the circuit and the combination of modulators and demodulators. 6AS6 pentodes are used as the time modulators. The duration of each gate pulse is 1/1600 sec. and one set of observations is obtained in 1/200 sec. One of the principal features of the present scheme is to use a common receiving system for all the components in order to avoid inevitable errors due to differences or changes in the gain and in the central frequencies of different receivers. A new type of square-law detector is employed in the present system [3]. It has rapid response time and excellent stability.

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References

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1. Hatanaka, T., Suzuki, S. and Tsuchiya, A. Proc. Japan Academy , 31, 81, 1955.
2. Hatanaka, T., Suzuki, S. and Tsuchiya, A. Publ. Astr. Soc. Japan , 7, 114, 1955.
3. Suzuki, S. Publ. Astr. Soc. Japan , 7, 121, 1955.
4. Hatanaka, T. Research Report EE-179, Cornell University, 1953.
5. Hatanaka, T. Research Report EE-257, Cornell University, 1955. Also Hatanaka, T. Publ. Astr. Soc. Japan, 8, 73, 1956.

68. Polarization of solar radio bursts

  • T. Hatanaka (a1)

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