Abstract
The Culgoora radioheliograph has been modified for observing at 327.4 MHz, which is in addition to the three frequencies (43.25, 80, and 160 MHz) previously available. At the new frequency the array beamwidth is 56″, which represents the highest resolution yet available for metre-wavelength solar mapping.
At 327.4 MHz the sources of radio emission are mainly in the lowest layers of the corona. Some preliminary four-frequency observations have been made of type I storms. It is found that the source size generally decreases with increasing observing frequency. This result confirms earlier suggestions that the sources of both type I and type III emission are contained in structures whose boundaries diverge outwards in the corona.
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Sheridan, K.V., Labrum, N.R., Payten, W.J. et al. Preliminary observations of solar radio sources with the Culgoora radioheliograph operating at four frequencies. Sol Phys 83, 167–177 (1983). https://doi.org/10.1007/BF00148251
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DOI: https://doi.org/10.1007/BF00148251