  The central engine of gamma-ray bursts (GRBs) is believed to eject
double-sided ultra-relativistic jets. For an observed GRB, one of the twin jets
should point toward us, and is responsible for the prompt gamma-ray and
subsequent afterglow emission. We consider in this Letter the other receding
jet, which will give rise to late-time radio re-brightening (RRB) when it
becomes non-relativistic (NR) and radiative isotropic. The RRB peaks at a time
$5t_{NR}=2(E_{j,51}/n)^{1/3}$ yr after the GRB, where $t_{NR}$ is the observed
NR timescale for the preceding jet, $E_j$ is the jet energy and $n$ is the
ambient medium density. The peak flux is comparable to the preceding-jet
emission at $t_{NR}$. We expect the RRB of GRB 030329 1.7 yr after the burst
with a flux $\sim0.6$ mJy at 15 GHz. The cases of GRBs 970508 and 980703 have
also been discussed. The detection of RRB, which needs dense monitoring
campaign even a few years after a GRB, will be the direct evidence for the
existence of double-sided jets in GRBs, and prove the black hole-disk system
formation in the cores of progenitors.
