Abstract
Monthly Notices of the Royal Astronomical Society 2015 454 (2):
1711-1718 The gamma-ray burst (GRB) jet powers the afterglow emission by shocking the
surrounding medium, and radio afterglow can now be routinely observed to almost
a year after the explosion. Long-duration GRBs are accompanied by supernovae
(SNe) that typically contain much more energy than the GRB jet. Here we
consider the fact that the SN blast wave will also produce its own afterglow
(supernova remnant emission), which will peak at much later time (since it is
non-relativistic), when the SN blast wave transitions from a coasting phase to
a decelerating Sedov-Taylor phase. We predict that this component will peak
generally a few tens of years after the explosion and it will outshine the GRB
powered afterglow well-before its peak emission. In the case of GRB 030329,
where the external density is constrained by the $\sim 10$-year coverage of the
radio GRB afterglow, the radio emission is predicted to start rising over the
next decade and to continue to increase for the following decades up to a level
of $\sim$ mJy. Detection of the SN-powered radio emission will greatly advance
our knowledge of particle acceleration in $ \sim 0.1$c shocks.