Neutron star asteroseismology and nuclear saturation parameter

Adopting various unified equations of state (EOSs), we examine the quasinormal modes gravitational waves from cold neutron stars. We focus on fundamental ($f$-), 1st pressure ($p_1$-), and spacetime ($w_1$-) modes, derive empirical formulae for frequencies damping rate those modes. With resultant formulae, find that value $\eta$, which is a specific combination nuclear saturation parameters, can be estimated within $\sim 30 \%$ accuracy, if $f$-mode frequency star whose mass known would observed or $f$- $p_1$-mode simultaneously observed, even though this estimation applicable only low-mass Additionally, radius canonical stars few per cent accuracy via simultaneous observations $w_1$-mode frequencies. also that, $f$-, $p_1$-, $2\%$ while $1\%$ with $M\ge 1.6M_\odot$ $0.6\%$ 1.4M_\odot$ constructed EOS constrained GW170817 event. Furthermore, strong correlation between maximum mass, minimum stellar compactness mass.