Within a minimum model for neutron stars consisting of nucleons , electrons and muons at \beta -equilibrium using about a dozen Equation of States ( EOSs ) from microscopic nuclear many-body theories and 40,000 EOSs randomly generated using an explicitly isospin-dependent parametric EOS model for high-density neutron-rich nucleonic matter within its currently known uncertainty range , we study correlations among the f-mode frequency , its damping time and the tidal deformability as well as the compactness of neutron stars .
Except for quark stars , both the f-mode frequency and damping time of canonical neutron stars are found to scale with the tidal deformability independent of the EOSs used .
Applying the constraint on the tidal deformability of canonical neutron stars \Lambda _ { 1.4 } = 190 ^ { +390 } _ { -120 } extracted by the LIGO+VIRGO Collaborations from their improved analyses of the GW170817 event , the f-mode frequency and its damping time of canonical neutron stars are limited to 1.67 kHz - 2.18 kHz and 0.155 s - 0.255 s , respectively , providing a useful guidance for the ongoing search for gravitational waves from the f-mode oscillations of isolated neutron stars .
Moreover , assuming either or both the f-mode frequency and its damping time will be measured precisely in future observations with advanced gravitational wave detectors , we discuss how information about the mass and/or radius as well as the still rather elusive nuclear symmetry energies at supra-saturation densities may be extracted .