Beta Decay and Nucleosynthesis in the Primordial Universe and in Neutron Stars

We study the electroweak processes in a hot and dense media. Electrons are the most significantly affected particles by the statistical background. This is due to their light mass, charge, and relativistic energy. Change in electron mass, charge, and wave function affects the production rate, through beta decay processes, and affects the interactions with other particles. We compute the change in electron self-mass, which ultimately affects the beta decay rate, and subsequently affects the change in helium abundance. We calculate this in two environments, which are the primordial universe and in neutron stars.