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The Polarization of Metre-Wave Solar Emission

Published online by Cambridge University Press:  25 April 2016

S. Suzuki  and
K. V. Sheridan
S. Suzuki
Affiliation:
Division of Radiophysics, CSIRO, Sydney
K. V. Sheridan
Affiliation:
Division of Radiophysics, CSIRO, Sydney
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Extract

Sources of the Type I storms are thought to lie on closed magnetic loop systems above bipolar sunspots. Usually one sunspot is stronger than the other in the bipolar magnetic structure, and accordingly only one radio source associated with the stronger sunspot is usually observed. Occasionally however a double radio source is observed in conjunction with the bipolar sunspots. In such a case the double radio source should be intrinsically bipolar, viz. the two components should emit opposite senses of circular polarization (in this paper we use the word polarity for simplicity).

Type
Contributions
Information
Publications of the Astronomical Society of Australia , Volume 4 , Issue 1 , 1980 , pp. 56 - 59
Copyright
Copyright © Astronomical Society of Australia 1980

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References

Benz, A. O., Urbarz, H., and Zlobec, P., Astron. Astrophys., 79, 216 (1979).Google Scholar
Cohen, M. H., Astrophys. J., 131, 664 (1960).Google Scholar
Dulk, G. A., and McLean, D. J., Solar Phys., 57, 279 (1978).Google Scholar
Duncan, R. A., Solar Phys., 63, 389 (1979).Google Scholar
Fokker, A. D., Doctoral Thesis, Leiden University (1960).Google Scholar
Kai, K., Solar Phys., 11, 456 (1970).Google Scholar
Labrum, N. R., and Stewart, R. T., Proc. Astron. Soc. Aust., 1, 316 (1970).Google Scholar
McLean, D. J., and Sheridan, K. V., Solar Phys., 26, 176 (1972).Google Scholar
Martyn, D. F., Nature, 158, 308 (1946).Google Scholar
Melrose, D. B., Proc. Astron. Soc. Aust., 2, 208 (1973).Google Scholar
Melrose, D. B., Aust. J. Phys., 27, 31 (1974).Google Scholar
Piddington, J. H., and Minnett, H. C., Aust. J. Sci. Res., A4, 131 (1951).Google Scholar
Saito, K., Ann. Tokyo Astron. Obs., Ser. 2, 12, 53 (1970).Google Scholar
Sheridan, K. V., McLean, D. J., and Smerd, S. F., Astrophys. Lett., 15, 139 (1973).Google Scholar
Stewart, R. T., Solar Phys., 50, 437 (1976).Google Scholar
Suzuki, S., Ann. Tokyo Astron. Obs., Ser. 2, 7, 75 (1961).Google Scholar
Suzuki, S., Solar Phys., 57, 415 (1978).Google Scholar
Suzuki, S., and Sheridan, K. V., Izv. Vyssh. Uchebn. Zaved. Radiofiz., 20, 1432 (1977) (English trans. Radiophys. Quant. Electron., 20, 989 (1978)).Google Scholar