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Aims: In this paper we study whether the shock-in-jet model, widely used toexplain the outbursting behaviour of quasars, can be used to explain the radioflaring behaviour of the microquasar Cygnus X-3.  Method: We have used a method developed to model the synchrotron outbursts ofquasar jets, which decomposes multifrequency lightcurves into a series ofoutbursts. The method is based on the Marscher & Gear (1985) shock model, butwe have implemented the modifications to the model suggested by Bjornsson &Aslaksen (2000), which make the flux density increase in the initial phase lessabrupt. We study the average outburst evolution as well as specificcharacteristics of individual outbursts and physical jet properties of Cyg X-3.  Results: We find that the lightcurves of the February-March 1994 andSeptember 2001 outbursts can be described with the modified shock model. Theaverage evolution shows that instead of the expected synchrotron plateau, theflux density is still increasing during the synchrotron stage. We also findthat high frequency peaking outbursts are shorter in duration than the onespeaking at lower frequencies. Finally, we show that the method can be used,complementary to radio interferometric jet imaging, for deriving the physicalparameters such as the magnetic field strength and the energy density ofrelativistic electrons in the jet of Cyg X-3.

Synchrotron flaring behaviour of CygnusX-3 during the February-March 1994 and September 2001 outbursts