Abstract
During observations of the star UV Ceti in Oct. 1963, radioemission was recorded on two frequencies that appears to have a different relationship with the visible flare. A pronounced time lag between the maximum of the optical flare and the maxima of the radioflares, and the time difference between the radio maxima on the two frequencies was compared with frequency drift type solar radio bursts A comparison of the major features of the UV Ceti flare with the mean values for the drift type solar bursts is tabulated. Available evidence both in regard to temporal relationships and spectra suggests that the flare on UV Ceti is analogous to the large solar noise storms or Type I bursts, whereas the other represents a much rarer type of event analogous to frequency drift solar bursts. (P.C.H)
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