  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.
