Abstract
The presence of free neutrons in relativistic outflows from compact ultra‐luminous objects alters their dynamical and radiative properties. The neutron‐proton decoupling at the acceleration phase produces energetic photons and neutrinos. In the magnetized outflows (e.g., MHD‐driven jets in hypernova‐like models), the decoupling is rather likely to convert the major part of outflow’s energy into neutrino emission. At the time of external shock formation, the interplay between primary and secondary (started by protons from neutron decay) shocks causes a reach variety of phenomena. These include appearance of one or more secondary peaks on a GRB or afterglow light‐curve, pre‐burst acceleration of ambient gas, bimodal distribution of GRB durations, etc.
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