  Considering the mass constraint from the resent pulsar observations, we study
the properties of neutron stars including hyperons and quarks explicitly. Using
the chiral quark-meson coupling model with relativistic Hartree-Fock
approximation, the equation of state (EoS) for hadronic matter is calculated by
taking into account the strange ($\sigma^{\ast}$ and $\phi$) mesons as well as
the light non-strange ($\sigma$, $\omega$, $\vec{\rho}$, and $\vec{\pi}$)
mesons in SU(3) flavor symmetry. On the other hand, the EoS for quark matter is
constructed with the simple MIT bag or the flavor-SU(3) Nambu-Jona-Lasinio
model, and we investigate the effect of the hadron-quark coexistence on the
neutron-star properties, imposing smooth crossover or Gibbs criterion for
chemical equilibrium. The mass-radius relation of a neutron star, as well as
physical quantities such as EoSs, particle fractions, and the speed of sound in
matter are presented. We find that, in order to prevent the quark appearance at
very low densities, the stiff hadronic EoS should be required under both of the
hadron-quark crossover and the first-order phase transition.

Nuclear Theory