  Taking into account the terrestrial experiments and the recent astrophysical
observations of neutron stars and gravitational-wave signals, we impose
restrictions on the equation of state (EoS) for isospin-asymmetric nuclear
matter. Using the relativistic mean-field model with SU(3) flavor symmetry, we
investigate the impacts of effective nucleon mass, nuclear incompressibility,
and slope parameter of nuclear symmetry energy on the nuclear and neutron-star
properties. It is found that the astrophysical information of massive neutron
stars and tidal deformabilities as well as the nuclear experimental data plays
an important role to restrict the EoS for neutron stars. Especially, the
softness of the nuclear EoS due to the existence of hyperons in the core gives
stringent constraints on those physical quantities. Furthermore, it is possible
to put limits on the curvature parameter of nuclear symmetry energy by means of
the nuclear and astrophysical calculations.
