2005MNRAS.364L..42F

We explore two possible models which might give rise to bright X-ray flares in gamma-ray burst (GRB) afterglows. One is an external forward-reverse shock model, in which the shock parameters of forward-reverse shocks are taken to be quite different. The other is a so-called `late internal-shock model', which requires a refreshed unsteady relativistic outflow generated after the prompt γ-ray emission. In the forward-reverse shock model, after the time t<sub>x</sub>at which the reverse shock crosses the ejecta, the flux declines more slowly than (t<sub>⊕</sub>/t<sub>x</sub>)<sup>–(2+β)</sup>, where t<sub>⊕</sub>denotes the observer's time and β is the spectral index of the X-ray emission. In the `late internal-shock model', decaying slopes much steeper than (t_⊕/t_e,⊕)^–(2+β) are possible if the central engine shuts down after t_e,⊕and the observed variability time-scale of the X-ray flare is much shorter than t_e,⊕.

The sharp decline of the X-ray flares detected in GRB 011121, XRF 050406, GRB 050502b and GRB 050730 rules out the external forward-reverse shock model directly and favours the `late internal-shock model'. These X-ray flares could thus hint that the central engine has begun to operate again and a new unsteady relativistic outflow is generated just a few minutes after the intrinsic hard burst.