The surprising influence of late charged current weak interactions on Big Bang Nucleosynthesis

The weak interaction charged current processes ($\nu_e+n\leftrightarrow p+e^-$,$\bar\nu_e +p\leftrightarrow n+e^+$,$n\leftrightarrow p+e^-+\bar\nu_e$) interconvert neutrons and protons in the early universe and have significant influence on Big Bang Nucleosynthesis (BBN) light-element abundance yields, particulary that for ${}^4\mathrm{H}\mathrm{e}$. We demonstrate that the influence of these processes is still significant even when they operate well below temperatures $T\sim 0.7\mathrm{M}\mathrm{e}\mathrm{V}$ usually invoked for “weak freeze-out,” and in fact down nearly into the alpha-particle formation epoch ($T \approx 0.1,{\rm MeV}$). This physics is correctly captured in commonly used BBN codes, though this late-time, low-temperature persistent effect of the isospin-changing weak processes, and the sensitivity of the associated rates to lepton energy distribution functions and blocking factors are not widely appreciated. We quantify this late-time influence by analyzing weak interaction rate dependence on the neutron lifetime, lepton energy distribution functions, entropy, the proton-neutron mass difference, and Hubble expansion rate. The effects we point out here render BBN a keen probe of any beyond-standard-model physics that alters lepton number/energy distributions, even subtly, in epochs of the early universe all the way down to near $T=100\mathrm{k}\mathrm{e}\mathrm{V}$.