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Candidate progenitor systems for Type Ia supernovae (SNe Ia) include double degenerate systems, cataclysmic variables, and symbiotic stars. In the symbiotic--star scenario a white dwarf accretes matter from the wind of a companion red giant, reaches the Chandrasekhar limit, and eventually explodes inside a circumstellar envelope formed by the stellar wind. We apply the circumstellar--interaction model for the radio emission developed by Chevalier to the symbiotic--star scenario. The main purpose is to predict the radio flux of SNe Ia and check if these objects may be detectable at radio wavelengths. We compare the predicted density of the circumstellar environment of the Type Ia progenitor star with the one typically expected in the case that the exploder is a white dwarf in a symbiotic system. This may provide a simple and effective test of the symbiotic--system scenario.
