By using the high resolution observations of Nançay observatory, we have been able to identify the S burst emission on the planetary radio astronomy (PRA) records of Voyager. It is shown that the S bursts occur in two regions of the ΦIO‐CML plane (S‐IoB and S‐IoA'C regions). In these regions the S burst emission is arranged into a pattern of repetitive features, drifting negatively. These features could be incomplete vertex late arcs. We show that the S burst pattern is distinct from the pattern of the Io‐controlled emission. These results are discussed in the frame of Goldstein and Thieman's arc model.
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Leblanc et al. (1981) studied this question.
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