Nucleosynthesis at Finite Temperature and Density
  We study the finite temperature and density effects on beta decay rates to
compute their contributions to nucleosynthesis in the early universe and
compact stars. We express nucleosynthesis parameters as a function of
temperature and density in different astronomical systems of interest. It is
explicitly shown that the chemical potential in the core of supermassive and
superdense stars affect beta decay and their helium abundance but the
background contributions is still dependent on relative temperature. We
calculate this contribution for temperature below the chemical potential. It
has been noticed that the acceptable background contribution are obtained for
comparatively larger values of T as temperature plays a role of regulating
parameter in an extremely dense system.
