  We discuss the results of a full relativistic treatment of the hydrodynamics
of disconnected quark regions during the final stages of the cosmological
quark-hadron transition. In this study, which represents a further development
of a previous analysis of the evaporation of cosmological quark drops, the
effects of long range energy and momentum transfer via electromagnetically
interacting particles are consistently taken into account. For this purpose, a
set of relativistic Lagrangian equations describing the evolution of the
strongly interacting fluids is coupled to a system of equivalent equations
accounting for the hydrodynamics of the fluid of electromagnetically
interacting particles. The complete set of equations has then been solved
numerically and results are presented from this. The inclusion of relativistic
radiative transfer produces significantly different results, with the formation
of high density regions at the end of the drop evaporation being particularly
relevant. A comparison is made with results obtained for the previous
radiation-free model and the cosmological implications concerning baryon number
concentrations are briefly discussed.
