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We explore the physics behind one of the brightest radio afterglows ever, GRB030329, at late times when the jet is non-relativistic. We determine thephysical parameters of the blast wave and its surroundings, in particular theindex of the electron energy distribution, the energy of the blast wave, andthe density (structure) of the circumburst medium. We then compare our resultswith those from image size measurements. We observed the GRB 030329 radioafterglow with the Westerbork Synthesis Radio Telescope and the Giant MetrewaveRadio Telescope at frequencies from 325 MHz to 8.4 GHz, spanning a time rangeof 268-1128 days after the burst. We modeled all the available radio data andderived the physical parameters. The index of the electron energy distributionis p=2.1, the circumburst medium is homogeneous, and the transition to thenon-relativistic phase happens at t_NR ~ 80 days. The energy of the blast waveand density of the surrounding medium are comparable to previous findings. Ourfindings indicate that the blast wave is roughly spherical at t_NR, and theyagree with the implications from the VLBI studies of image size evolution. Itis not clear from the presented dataset whether we have seen emission from thecounter jet or not. We predict that the Low Frequency Array will be able toobserve the afterglow of GRB 030329 and many other radio afterglows,constraining the physics of the blast wave during its non-relativistic phaseeven further.

Detailed study of the GRB 030329 radio afterglow deep into the non-relativistic phase