Abstract
The radio astronomical studies of solar activity are powerful complementary tools to the studies in the other parts of the electromagnetic spectrum and of the corpuscular emissions. We can either observe the Solar radio emission directly or resort to the occultation techniques. The solar radio emission is monitored world wide in all the radio bands, both as the quiet Sun and the bursty solar radio events which can reach levels up to about one million times over the quiet Sun radio emission level. The solar cycle is very much more pronounced in the bursty than it is in the quiet solar emission. The four decades of solar coronal scattering observations have given us extensive information about the varying conditions in the solar outer corona as well as in the remote regions of the heliosphere (by means of the interplanetary scintillation technique). In addition the radio observations have the important advantage which permits us to study the Jovian magnetosphere at the decimetre wavelength all the time from the ground based radio observatories, where it was first discovered more than a decade before the first independent Pioneer and later by the Voyager spacecraft confirmations. Due to the effect of the 22 year solar magnetic cycle which reverses the magnetic polarity of the Sun an unexpected decline has been observed in the late 60-ties and early 70-ties of the scattering of radio waves in the Solar Corona. During the same time there was also a marked decline of the radio emission from the Jovian magnetosphere. This 30% fall of the Jovian decimetric radio emission recovered within several years.
Published Version
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