Neutron Star Equation of State in Two-fluid Formalism

Abstract

The neutron star is a compact astrophysical object with extreme gravity and magnetic fields. We can hypothesize the internal structure of the neutron star due to the observed phenomena. One such phenomenon is the glitches observed in pulsars, which can be a probe for the superfluid dynamics of neutron stars. In this thesis, we are trying to look at various superfluid models. We have used Quantum Hadrodynamics to define the star’s internal composition and the density dependent model to generate EoS to define a Neutron star for the superfluid state. We also used the EoS to generate a Mass radius plot for Tolman-Oppenheimer-Volkoff equations and compare it with the observational pulsar data. We will also use the Thorne-Hartle approximation to determine the Fractional Moment of Inertia in a slow-rotating neutron star. We have derived the entrainment parameter and effective mass. This EoS in the two-fluid formalism will help to understand the irregular rotations and pulsar glitches in the future.