  Neutron star (NS) is a unique astronomical compact object where the four
fundamental interactions have been revealed from the observation and studied in
different ways. While the macroscopic properties of NS like mass and radius can
be determined within the General Relativity using a realistic equation of state
(EOS) of NS matter, such an EOS is usually generated by a nuclear structure
model like, e.g., the nuclear mean-field approach to asymmetric nuclear matter.
Given the radius of NS extended to above 10 km and its mass up to twice the
solar mass, NS is expected to be tidally deformed when it is embedded in a
strong tidal field. Such a tidal effect was confirmed unambiguously in the
gravitation wave signals detected recently by the LIGO and Virgo laser
interferometers from GW170817, the first ever direct observation of a binary NS
merger. A nonrelativistic mean-field study is carried out in the present work
within the Hartree-Fock formalism to construct the EOS of NS matter, which is
then used to determine the tidal deformability, gravitational mass, and radius
of NS. The mean-field results are compared with the constraints imposed for
these quantities by the global analysis of the observed GW170817 data, and a
strong impact by the incompressibility of nuclear matter on the hydrostatic
configuration of NS is shown.
