THE OBSERVED SIZE AND SHAPE OF GAMMA-RAY BURST AFTERGLOW

The detection of delayed emission in X-ray, optical, and radio wavelen gth, or ''afterglow,'' following a gamma-ray burst can be described as the emission of a relativistic shell decelerating upon collision with the interstellar medium. We show that the observed radiation surface has well-defined bright edges. We derive an explicit expression for th e size as a function of time, and obtain the surface brightness distri bution. This might be directly observed if the burst occurs at a small redshift so that its radio signal can be resolved. The size and shape are relevant for detailed analysis of scintillation or microlensing. We show that the effective Lorentz factor depends on the observed freq uency and that it is higher for frequencies above the synchrotron typi cal frequency (optical and X-ray) than for low frequencies (radio). Co nsequently, transition to nonrelativistic evolution will be observed f irst in low frequencies and only a factor of similar to 2 later in the high frequencies.