The composition and equation of state of a perfect gas of photons, electrons-photons, neutrinos, and nucleons is calculated under the assumption of either perfect neutrino transparency or some buildup of neutrino concentration in dense matter. The calculations are applicable to collapsing stars after thermal dissociation (temperatures above 10 billion K) and before nuclear forces are important (densities below 10 to the 14th power g/cu cm).
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Riper et al. (1977) studied this question.