We have identified two GRBs in which early emission is very different than late emission. Post‐quiescent pulses of BATSE GRBs 960530 and 980125 have long lags, smooth morphologies, and soft spectral evolution. The early emission satisfies the standard internal shock paradigm, while the late emission is consistent with external shocks. The peak luminosity ratio between early and late episodes is not in agreement with that predicated by the lag vs. peak luminosity relationship. We briefly discuss these observations in terms of a current hypernova jet model. © 2004 American Institute of Physics