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Neutron star properties, such as its mass, radius, and moment of inertia, arecalculated by solving the Tolman-Oppenheimer-Volkov (TOV) equations using thering-diagram equation of state (EOS) obtained from realistic low-momentum NNinteractions $V_{low-k}$. Several NN potentials (CDBonn, Nijmegen, Argonne V18and BonnA) have been employed to calculate the ring-diagram EOS where theparticle-particle hole-hole ring diagrams are summed to all orders. The protonfractions for different radial regions of a $\beta$-stable neutron star aredetermined from the chemical potential conditions $\mu_n-\mu_p = \mu_e =\mu_\mu$. The neutron star masses, radii and moments of inertia given by theabove potentials all tend to be too small compared with the accepted values.Our results are largely improved with the inclusion of medium corrections basedon Brown-Rho scaling where the in-medium meson masses, particularly those of$\omega$, $\rho$ and $\sigma$, are slightly decreased compared with theirin-vacuum values. Representative results using such medium correctedinteractions are neutron star mass $M\sim 1.8 M_{\odot}$, radius $R\sim 9$ kmand moment of inertia $\sim 60 M_{\odot}km^2$. The mass-radius trajectoriesgiven by the above four realistic NN potentials are by and large overlapping.

Neutron star, $\beta$-stable ring-diagram equation of state and Brown-Rho scaling