Abstract
THE system III (1957) decametric rotation period of Jupiter, based on observations of the decametric radiation between 1951 and 1960, was defined by Douglas and Smith1 and Smith et al.2. They found, however, that the central meridian longitude (CML) of the source A (200<CML<280) exhibited a marked drift towards higher longitudes in the years following 1961. Guilds and Carr3 and Donivan and Carr4 showed that an increase of the rotation period by 0.30 s changed this drift into a sinusoidal variation of the source A position, thus defining a new CML system—system III (1967). The sinusoidal curve has a period of about 11 yr and the period of Jupiter's orbital motion about the Sun is 11.86 yr, Donivan and Carr4 showed that the variation of the source A position is closely related to the change in Jovicentric declination of the Earth (DE), whereas the correlation (or rather anticorrelation) of the source A position with sunspot number is poor.
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References
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Axford, W. I., and Hines, C. O., Canad. J. Phys., 39, 1433 (1961).
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GOERTZ, C. Variation of Source A Position of the Jovian Decametric Radiation. Nature Physical Science 229, 151–152 (1971). https://doi.org/10.1038/physci229151a0
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DOI: https://doi.org/10.1038/physci229151a0
