All Tables

Table 1: Properties of isolated static neutron stars of gravitational mass $M=1.35~{M}_\odot$ for the three EOSs used in our computations. $M/R\equiv GM/Rc^2$ is the compaction parameter, R is the areal radius, $M_{\rm B}$ is the baryon mass and $\rho _{\rm c}$ is the central energy density, respectively.
Table 2: Parameters of polynomial fits (7) and (9).
Table 3: Gravitational wave frequencies (in Hz) computed from the calculated data for GNH3, APR and BPAL12 EOSs: the $f_{\rm npm}$ denotes the frequency at which the non-point-mass effects start to be important, $f_{\rm 20}, f_{\rm 25}$ and $f_{\rm 40}$ are the so-called break-frequencies (see text), whereas $f_{\rm end}$ is the GW frequency on the final orbit.
Table 4: Pressure coefficient $\kappa$ , adiabatic index $\gamma$ and baryon mass $M_{\rm B}$ for polytropic NSs having the same compactness parameter and mass ( $M=1.35~{M}_\odot$ ) than NSs described by realistic EOSs (Table 1) ( $\hat{\rho}:=1.66$ $\times$ $10^{14}~{\rm g/cm^3}$ and $\hat{n}:=0.1~{\rm fm^{-3}}$ ).