  Based on an equivparticle model, we investigate the in-medium quark
condensate in neutron stars. Carrying out a Taylor expansion of the nuclear
binding energy to the order of $\rho^3$, we obtain a series of EOSs for neutron
star matter, which are confronted with the latest nuclear and astrophysical
constraints. The in-medium quark condensate is then extracted from the
constrained properties of neutron star matter, which decreases non-linearly
with density. However, the chiral symmetry is only partially restored with
non-vanishing quark condensates, which may vanish at a density that is out of
reach for neutron stars.
