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We calculate the evolution of the early universe through the epochs of weakdecoupling, weak freeze-out and big bang nucleosynthesis (BBN) bysimultaneously coupling a full strong, electromagnetic, and weak nuclearreaction network with a multi-energy group Boltzmann neutrino energy transportscheme. The modular structure of our code provides the ability to dissect therelative contributions of each process responsible for evolving the dynamics ofthe early universe in the absence of neutrino flavor oscillations. Such anapproach allows a detailed accounting of the evolution of the $\nu_e$,$\bar\nu_e$, $\nu_\mu$, $\bar\nu_\mu$, $\nu_\tau$, $\bar\nu_\tau$ energydistribution functions alongside and self-consistently with the nuclearreactions and entropy/heat generation and flow between the neutrino andphoton/electron/positron/baryon plasma components. This calculation revealsnonlinear feedback in the time evolution of neutrino distribution functions andplasma thermodynamic conditions (e.g., electron-positron pair densities), withimplications for: the phasing between scale factor and plasma temperature; theneutron-to-proton ratio; light-element abundance histories; and thecosmological parameter \neff. We find that our approach of following the timedevelopment of neutrino spectral distortions and concomitant entropy productionand extraction from the plasma results in changes in the computed value of theBBN deuterium yield. For example, for particular implementations of quantumcorrections in plasma thermodynamics, our calculations show a $0.4\%$ increasein deuterium. These changes are potentially significant in the context ofanticipated improvements in observational and nuclear physics uncertainties.

Neutrino energy transport in weak decoupling and big bang nucleosynthesis