Thermal Contributions to Primordial Nucleosynthesis

Electron mass is known to modify at finite temperatures and densities. Weak nuclear processes have a great impact on electron mass which modifies in a statistical background. We demonstrate how the temperature change in electron mass is associated with beta decay in the early universe. Its precise contributions to the abundance of light elements in the early universe describe some of the details about nucleosynthesis. We employ the calculational scheme of the renormalization of QED to precisely compute the temperature dependence of electron mass during the nuclear processes. In this paper we precisely compute the concentration of electron and its mass change with temperature during nucleosynthesis and use it to describe the helium abundance, expansion rate and energy density of the universe during nucleosynthesis.