Gamma-ray burst afterglow: Polarization and analytic light curves

Gamma-ray burst afterglow polarization is discussed. We find an observable, up to similar to 10%, polarization, if the magnetic held coherence length grows at about the speed of light after the field is generated at the shock front. Detection of a polarized afterglow would show that collisionless ul trarelativistic shocks can generate strong large-scale magnetic fields and confirm the synchrotron afterglow model. Nondetection, at the similar to 1% level, would imply that either the synchrotron emission model is incorrect or that strong magnetic fields, after they are generated in the shock, som ehow manage to stay undissipated at "microscopic," skin depth, scales. Anal ytic light curves of synchrotron emission from an ultrarelativistic self-si milar blast wave are obtained for an arbitrary electron distribution functi on, taking into account the effects of synchrotron cooling. The peak synchr otron flux and the flux at frequencies much smaller than the peak frequency are insensitive to the details of the electron distribution function; henc e, their observational determination would provide strong constraints on bl ast-wave parameters.