  We have observed a number of minor radio flares in Cyg X-3 using the MERLIN
array. Photometric observations show the system to be highly active with
multiple flares on hourly timescales over the one month observing programme.
Analysis of the source's power spectrum show no persistent periodicities in
these data, and no evidence of the 4.8 hr orbital period. An upper limit of 15
mJy can be placed on the amplitude of any sinusoidal varaition of source flux
at the orbital period. The brightness temperature of a flare is typically T >
10^{9}- 10^{10} K, with a number of small flares of 5 minute duration having
brightness temperatures of T > few x 10^{11} K. For such a change in flux to
occur within a typical 10 minute timescale, the radiation must originate from
plasmons with a size < 1.22 AU. This emission is unlikely to originate close to
the centre of the system as both the jets and compact object are buried deep
within an optically thick stellar wind. Assuming a spherically symmetric wind,
plasmons would become visible at distances ~ 13 AU from the core.
