Abstract
The two-element interferometer at Hat Creek Observatory was used at 1.3 cm wavelength to study the fine structure of the radio emissive regions on the Sun. Observations of the quiet Sun at 1.3 cm show sudden changes in the fringe amplitude and phase, lasting for typically about 5–8 min. Assuming that these events are identical in nature, a plot of peak amplitude vs the projected baseline at the time of the event suggests emission from a region of angular size of about 10″. The corresponding brightness temperature is 50000 K. It is possible that these events may be related to the appearance and disappearance of groups of spicules or mottles.
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References
Beckers, J. M.: 1972, Ann. Rev. Astron. Astrophys. 10, 73.
Hills, R., Janssen, M., Thornton, D. D., and Welch, W. J.: 1973, IEEE Special Issue on Radio and Radar Astronomy, in press.
Leighton, R. B., Noyes, R. W., and Simon, G. W.: 1962, Astrophys. J. 135, 474.
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Kundu, M.R., Velusamy, T. Fine structure of the Sun at 1.3 cm wavelength. Sol Phys 34, 125–131 (1974). https://doi.org/10.1007/BF00149604
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DOI: https://doi.org/10.1007/BF00149604