Compact Stars With Vacuum Fluctuations

As supernova products, neutron stars with the extreme conditions of high density, strong gravitational field and electromagnetic field are unique cosmic physics laboratory, which has been highly favored by physicists and astrophysicists. In this thesis, we will investigate the asymmetric neutron stars consisting of neutrons, proton, and leptons. Our work is based on FSUGold model and relativistic mean field theory (RMF). We calculate the effective masses of nucleons and mesons in relativistic Hartree approximation (RHA) and random phase approximation (RPA). The equations of states (EOS) are then calculated by taking into account the effects of vacuum fluctuations (VF). Substituting the EOS into Tolman-Oppenheimer-Volkoff (TOV) equation, we calculate the maximum mass of the neutron stars, which was reduced from 1.71 Msum to 1.35Msum (pr1.40Msun) by fitting three (or five) parameters at nuclear saturation. Meanwhile, various properties of the neutron stars are shown to be "softened" comparing to that obtained in the FSUGold. Compared with the new observation data from astronomy, it seems that high order loop contributions and other physical mechanisms contribution remains to be studied within the relativistic mean field theory framework.