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 5 t _ { 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 \sim 0.6 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 .