The evolution of GRB remnants

Abstract

The detection of the delayed emission in X-ray, optical and radio band, i.e. the afterglow of $γ$-ray bursts (GRBs), suggestes that the sources of GRBs are likely to be at cosmological distances. Here we explore the interaction of a relativistic shell with a uniform interstellar medium (ISM) and obtain the exact solution of the evolution of $γ$-ray burst remnants, including the radiative losses. We show that in general the evolution of bulk Lorentz factor $γ$ satisfies $γ\propto t^{-α_{t}}$ when $γ\gg 1$, here $α_{t}$ is mainly in the range $9/22 \sim 3/8$, the latter corresponds to adiabatic expansion. So it is clear that adiabatic expansion is a good approximation even when radiative loss is considered. However, in fact, $α_{t}$ is slightly larger than 3/8, which may have some effects on a detailed data analysis. Synchrotron-self-absorption is also calculated and it is demonstrated that the radio emission may become optically thin during the afterglow. Our solution can also apply to the nonrelativistic case ($γ\sim 1$), at that time the observed flux decrease more rapidly than that in the relativistic case.