2003MNRAS.339..881R

In models for γ-ray burst afterglows, it is normally assumed that the external shock strongly amplifies the magnetic field and that this field maintains a steady value throughout the shocked region. We discuss the effects of modifying this (probably simplistic) assumption by allowing for a short decay time. The observations are incompatible with a post-shock field that decays too rapidly. However, if the field pervades only a few per cent of the total thickness of the shocked shell (and the electrons undergo only inverse Compton losses in the remainder), the model could be compatible with data. This would suggest a strong dependence of model parameters on the uncertainties of shock physics, therefore calling for independent external density estimates. We claim that afterglow emission should be instead seen as a laboratory where we can understand relativistic shock physics. The model we propose here together with afterglow observations in all wavebands could help to pin down the field structure.