The standard theory of this process, whose product distribution was posited to be dependent on neutron capture cross section rather than stability in the Alpher-Bethe-Gamow paper, predicts an exquisite dependence on the baryon-to-photon and neutron-to-proton ratios and predicts a mass abundance of around 25% for helium.  
This process can be simulated using the Kawano-Wagoner code. A nonstandard theory of this process by Kneller and Stiegman in which there is additional relativistic energy incorporates a "speedup factor". The timescale of this process limits the number of neutrino families to 3. Fermi and Turkevich determined that this process has "crevasses" at A equals 5 and A equals 8. The ratios of the precursors to this process were fixed to a 1 to 6 ratio by the freezing-out of weak interactions. The first product of this process is easily disrupted by high-energy photons because of its 2.2 MeV binding energy, leading to that product's namesake (*) bottleneck. The standard theory of this process, whose product distribution was posited to be dependent on neutron capture cross section rather than stability in the Alpher-Bethe-Gamow paper, predicts an exquisite dependence on the baryon-to-photon and neutron-to-proton ratios and predicts a mass abundance of around 25% for helium.  For 10 points, name this process that occurred between 3 and 20 minutes after the start of the universe, in which light elements were created.
This process can be simulated using the Kawano-Wagoner code.
big bang nucleosynthesis [or BBN, or primordial nucleosynthesis; prompt on partial answer]