Helium formation during nucleosynthesis was limited by the initial abundance of free neutrons, which were necessary for creating deuterium, a precursor to helium. The early universe had a proton-to-neutron ratio of about 7 to 1, leading to a rapid consumption of free neutrons to form deuterium, leaving predominantly hydrogen. The fusion of protons into deuterium is rare due to the weak interaction, making it difficult for helium to form without sufficient deuterium. Consequently, the short timeframe of Big Bang Nucleosynthesis (BBN) further restricted helium production, as the universe cooled quickly. A higher neutron-to-proton ratio would have resulted in significantly more helium being produced during this process.