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Solar Radio Observations at 843 MHz

Published online by Cambridge University Press:  25 April 2016

A. D. Gray ,
D. Campbell-Wilson  and
M. I. Large
A. D. Gray
Affiliation:
School of Physics, University of Sydney
D. Campbell-Wilson
Affiliation:
School of Physics, University of Sydney
M. I. Large
Affiliation:
School of Physics, University of Sydney
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Abstract

The Molonglo Observatory Synthesis Telescope (MOST) has been used to observe the Sun with total-power fan-beams having a one-dimensional resolution of 41 arcsec at 843 MHz. The scans reveal clearly the rotation and evolution of the slowly-varying component as well as some burst activity. Low radio brightness features have also been identified, but the exact relationship between these features and coronal holes is, as yet, unclear. Several partial synthesis observations have been used to generate two-dimensional radioheliograms.

Information

Type
Solar
Information
Publications of the Astronomical Society of Australia , Volume 8 , Issue 2 , 1989 , pp. 142 - 144
Copyright
Copyright © Astronomical Society of Australia 1989

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References

Allen, C. W., 1973, Astrophyskal Quantities (3rd edition), (TheAthlone Press, 1973).Google Scholar
Chiuderi, C., Chiuderi Drago, F. and Noci, G., 1972, SolarPhys., 26, 343.Google Scholar
Christiansen, W. N. and Warburton, J. A., 1953, Aust. J. Phys., 6, 262.CrossRefGoogle Scholar
Christiansen, W. N., Warburton, J. A. and Davies, R. D., 1957, Aust. J. Phys., 10, 491.Google Scholar
Crawford, D. F., 1984, in Roberts, J. A. (e.d), Proc. URSI/IAUSymp. Indirect Imaging, 373, (Cambridge University Press, 1984).Google Scholar
Dulk, G. A., 1988, private communications.Google Scholar
Ferguson, B. G., 1981, Solar Phys., 69, 185.Google Scholar
Kundu, M. R., 1965, Solar Radio Astronomy, (Interscience Publishers, Wiley and Sons, 1965).Google Scholar
Melrose, D.B., 1985, in McLean, D. J. and Labrum, N. R. (eds.), Solar Radiophysics, (Cambridge University Press, 1985).Google Scholar
Mills, B. Y., 1981, Proc. Astron. Soc. Aust., 4, 156.Google Scholar
Papagiannis, M. D. and Baker, K.B., 1982, Solar Phys., 79, 365.Google Scholar
Thompson, A. R., Moran, J. M. and Swenson, G. W. Jr., Interferometry and Synthesis in Radio Astronomy, (Wiley and Sons, 1986).Google Scholar