Abstract
We have constructed and compared models of rotating neutron stars and strange stars, within the Hartle framework. The significance of the low energy density region and crust region inside the neutron star has been studied, along with how much the existence of strange matter above the energy density 300 MeV/fm3 can affect the neutron star properties. We have confirmed several universalities among the neutron star properties such as, dimensionless moment of inertia vs dimensionless quadrupole moment, dimensionless tidal deformability vs dimensionless moment of inertia and moment of inertia parameters vs R/2M.
Highlights
From the atmosphere to the core of neutron stars covers an energy density range from 106 gm/cm3 to several times nuclear matter density
The strange matter Equation of state (EoS) around the energy density 300 MeV/fm3 and 500 MeV/fm3 crosses the nucleons only matter EoS, suggesting a transition to strange quark matter often called a ”strange star”
N-QMC700 is the stiffest EoS which is based on nucleon only matter
Summary
From the atmosphere to the core of neutron stars covers an energy density range from 106 gm/cm3 to several times nuclear matter density. We will compare properties of neutron stars based on EoSs that include either, nucleons only, nucleons and hyperons or strange quark matter at high energy density.
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